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Title: The Heavens Above: A Popular Handbook of Astronomy

Author: J. A. Gillet
        W. J. Rolfe

Release date: February 2, 2019 [eBook #58810]

Language: English

Credits: E-text prepared by Colin Bell, Brenda Lewis, David King, and the Online Distributed Proofreading Team (http://www.pgdp.net) from page images generously made available by Internet Archive (https://archive.org)


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[Illustration: SPECTRA OF VARIOUS SOURCES OF LIGHT.]

           The Heavens Above: A Popular Handbook of Astronomy


THE HEAVENS ABOVE:

A Popular Handbook of Astronomy.

by

J. A. GILLET,

Professor of Physics in the Normal College of the City of New York,

and

W. J. ROLFE,

Formerly Head Master of the High School, Cambridge, Mass.

With Six Lithographic Plates and Four Hundred
and Sixty Wood Engravings.






Potter, Ainsworth, & Co.,
New York and Chicago.
1882.

Copyright by
J. A. Gillet and W. J. Rolfe,
1882.

Franklin Press:
Rand, Avery, and Company,
Boston.




                                PREFACE.


It has been the aim of the authors to give in this little book a brief,
simple, and accurate account of the heavens as they are known to
astronomers of the present day. It is believed that there is nothing in
the book beyond the comprehension of readers of ordinary intelligence,
and that it contains all the information on the subject of astronomy
that is needful to a person of ordinary culture. The authors have
carefully avoided dry and abstruse mathematical calculations, yet they
have sought to make clear the methods by which astronomers have gained
their knowledge of the heavens. The various kinds of telescopes and
spectroscopes have been described, and their use in the study of the
heavens has been fully explained.

The cuts with which the book is illustrated have been drawn from all
available sources; and it is believed that they excel in number,
freshness, beauty, and accuracy those to be found in any similar work.
The lithographic plates are, with a single exception, reductions of the
plates prepared at the Observatory at Cambridge, Mass. The remaining
lithographic plate is a reduced copy of Professor Langley's celebrated
sun-spot engraving. Many of the views of the moon are from drawings made
from the photographs in Carpenter and Nasmyth's work on the moon. The
majority of the cuts illustrating the solar system are copied from the
French edition of Guillemin's "Heavens." Most of the remainder are from
Lockyer's "Solar Physics," Young's "Sun," and other recent authorities.
The cuts illustrating comets, meteors, and nebulæ, are nearly all taken
from the French editions of Guillemin's "Comets" and Guillemin's
"Heavens."




                               CONTENTS.


I. THE CELESTIAL SPHERE 3

II. THE SOLAR SYSTEM 41

    I. THEORY OF THE SOLAR SYSTEM 41

        The Ptolemaic System 41

        The Copernican System 44

        Tycho Brahe's System 44

        Kepler's System 44

        The Newtonian System 48

    II. THE SUN AND PLANETS 53

        I. The Earth 53

            Form and Size 53

            Day and Night 57

            The Seasons 64

            Tides 68

            The Day and Time 74

            The Year 78

            Weight of the Earth and Precession 83

        II. The Moon 86

            Distance, Size, and Motions 86

            The Atmosphere of the Moon 109

            The Surface of the Moon 114

    III. Inferior and Superior Planets 130

        Inferior Planets 130

        Superior Planets 134

    IV. The Sun 140

        I. Magnitude and Distance of the Sun 140

        II. Physical and Chemical Condition of the Sun 149

            Physical Condition of the Sun 149

            The Spectroscope 152

            Spectra 158

            Chemical Constitution of the Sun 164

            Motion at the Surface of the Sun 168

        III. The Photosphere and Sun-Spots 175

            The Photosphere 175

            Sun-Spots 179

        IV. The Chromosphere and Prominences 196

        V. The Corona 204

    V. Eclipses 210

    VI. The Three Groups of Planets 221

        I. General Characteristics of the Groups 221

        II. The Inner Group of Planets 225

            Mercury 225

            Venus 230

            Mars 235

        III. The Asteroids 241

        IV. Outer Group of Planets 244

            Jupiter 244

                The Satellites of Jupiter 250

            Saturn 255

                The Planet and his Moons 255

                The Rings of Saturn 261

            Uranus 269

            Neptune 271

    VII. Comets and Meteors 274

        I. Comets 274

            General Phenomena of Comets 274

            Motion and Origin of Comets 281

            Remarkable Comets 290

            Connection between Meteors and Comets, 300

            Physical and Chemical Constitution of Comets 314

        II. The Zodiacal Light 318

III. THE STELLAR UNIVERSE 322

    I. General Aspect of the Heavens 322

    II. The Stars 330

        The Constellations 330

        Clusters 350

        Double and Multiple Stars 355

        New and Variable Stars 358

        Distance of the Stars 364

        Proper Motion of the Stars 365

        Chemical and Physical Constitution of the Stars 371

    III. Nebulæ 373

        Classification of Nebulæ 373

        Irregular Nebulæ 376

        Spiral Nebulæ 384

        The Nebular Hypothesis 391

    IV. The Structure of the Stellar Universe 396




                                   I.
                         THE CELESTIAL SPHERE.


I. _The Sphere._--A _sphere_ is a solid figure bounded by a surface
which curves equally in all directions at every point. The rate at which
the surface curves is called the _curvature_ of the sphere. The smaller
the sphere, the greater is its curvature. Every point on the surface of
a sphere is equally distant from a point within, called the _centre_ of
the sphere. The _circumference_ of a sphere is the distance around its
centre. The _diameter_ of a sphere is the distance through its centre.
The _radius_ of a sphere is the distance from the surface to the centre.
The surfaces of two spheres are to each other as the squares of their
radii or diameters; and the volumes of two spheres are to each other as
the cubes of their radii or diameters.

Distances on the surface of a sphere are usually denoted in _degrees_. A
degree is 1/360 of the circumference of the sphere. The larger a sphere,
the longer are the degrees on it.

A curve described about any point on the surface of a sphere, with a
radius of uniform length, will be a circle. As the radius of a circle
described on a sphere is a curved line, its length is usually denoted in
degrees. The circle described on the surface of a sphere increases with
the length of the radius, until the radius becomes 90°, in which case
the circle is the largest that can possibly be described on the sphere.
The largest circles that can be described on the surface of a sphere are
called _great circles_, and all other circles _small circles_.

    Any number of great circles may be described on the surface of a
    sphere, since any point on the sphere may be used for the centre of
    the circle. The plane of every great circle passes through the
    centre of the sphere, while the planes of all the small circles pass
    through the sphere away from the centre. All great circles on the
    same sphere are of the same size, while the small circles differ in
    size according to the distance of their planes from the centre of
    the sphere. The farther the plane of a circle is from the centre of
    the sphere, the smaller is the circle.

    By a _section_ of a sphere we usually mean the figure of the surface
    formed by the cutting; by a _plane section_ we mean one whose
    surface is plane. Every plane section of a sphere is a circle. When
    the section passes through the centre of the sphere, it is a great
    circle; in every other case the section is a small circle. Thus,
    _AN_ and _SB_ (Fig. 1) are small circles, and _MM'_ and _SN_ are
    large circles.

[Illustration: Fig. 1.]

    In a diagram representing a sphere in section, all the circles whose
    planes cut the section are represented by straight lines. Thus, in
    Fig. 2, we have a diagram representing in section the sphere of Fig.
    1. The straight lines _AN_, _SB_, _MM'_, and _SN_, represent the
    corresponding circles of Fig. 1.

The _axis_ of a sphere is the diameter on which it rotates. The _poles_
of a sphere are the ends of its axis. Thus, supposing the spheres of
Figs. 1 and 2 to rotate on the diameter _PP'_, this line would be called
the axis of the sphere, and the points _P_ and _P'_ the poles of the
sphere. A great circle, MM', situated half way between the poles of a
sphere, is called the _equator_ of the sphere.

Every great circle of a sphere has two poles. These are the two points
on the surface of the sphere which lie 90° away from the circle. The
poles of a sphere are the poles of its equator.

[Illustration: Fig. 2.]

2. _The Celestial Sphere._--The heavens appear to have the form of a
sphere, whose centre is at the eye of the observer; and all the stars
seem to lie on the surface of this sphere. This form of the heavens is a
mere matter of perspective. The stars are really at very unequal
distances from us; but they are all seen projected upon the celestial
sphere in the direction in which they happen to lie. Thus, suppose an
observer situated at _C_ (Fig. 3), stars situated at _a_, _b_, _d_, _e_,
_f_, and _g_, would be projected upon the sphere at _A_, _B_, _D_, _E_,
_F_, and _G_, and would appear to lie on the surface of the heavens.

[Illustration: Fig. 3.]

3. _The Horizon._--Only half of the celestial sphere is visible at a
time. The plane that separates the visible from the invisible portion is
called the _horizon_. This plane is tangent to the earth at the point of
observation, and extends indefinitely into space in every direction. In
Fig. 4, _E_ represents the earth, _O_ the point of observation, and _SN_
the horizon. The points on the celestial sphere directly above and below
the observer are the poles of the horizon. They are called respectively
the _zenith_ and the _nadir_. No two observers in different parts of the
earth have the same horizon; and as a person moves over the earth he
carries his horizon with him.

[Illustration: Fig. 4.]

The dome of the heavens appears to rest on the earth, as shown in Fig.
5. This is because distant objects on the earth appear projected against
the heavens in the direction of the horizon.

[Illustration: Fig. 5.]

The _sensible_ horizon is a plane tangent to the earth at the point of
observation. The _rational_ horizon is a plane parallel with the
sensible horizon, and passing through the centre of the earth. As it
cuts the celestial sphere through the centre, it forms a great circle.
_SN_ (Fig. 6) represents the sensible horizon, and _S'N'_ the rational
horizon. Although these two horizons are really four thousand miles
apart, they appear to meet at the distance of the celestial sphere; a
line four thousand miles long at the distance of the celestial sphere
becoming a mere point, far too small to be detected with the most
powerful telescope.

[Illustration: Fig. 6.]

[Illustration: Fig. 7.]

4. _Rotation of the Celestial Sphere._--It is well known that the sun
and the majority of the stars rise in the east, and set in the west. In
our latitude there are certain stars in the north which never disappear
below the horizon. These stars are called the _circumpolar_ stars. A
close watch, however, reveals the fact that these all appear to revolve
around one of their number called the _pole star_, in the direction
indicated by the arrows in Fig. 7. In a word, the whole heavens appear
to rotate once a day, from east to west, about an axis, which is the
prolongation of the axis of the earth. The ends of this axis are called
the _poles_ of the heavens; and the great circle of the heavens, midway
between these poles, is called the _celestial equator_, or the
_equinoctial_. This rotation of the heavens is apparent only, being due
to the rotation of the earth from west to east.

5. _Diurnal Circles._--In this rotation of the heavens, the stars appear
to describe circles which are perpendicular to the celestial axis, and
parallel with the celestial equator. These circles are called _diurnal
circles_. The position of the poles in the heavens and the direction of
the diurnal circles with reference to the horizon, change with the
position of the observer on the earth. This is owing to the fact that
the horizon changes with the position of the observer.

[Illustration: Fig. 8.]

When the observer is north of the equator, the north pole of the heavens
is _elevated_ above the horizon, and the south pole is _depressed_ below
it, and the diurnal circles are _oblique_ to the horizon, leaning to the
south. This case is represented in Fig. 8, in which _PP'_ represents the
celestial axis, _EQ_ the celestial equator, _SN_ the horizon, and _ab_,
_cN_, _de_, _fg_, _Sh_, _kl_, diurnal circles. _O_ is the point of
observation, _Z_ the zenith, and _Z'_ the nadir.

[Illustration: Fig. 9.]

When the observer is south of the equator, as at _O_ in Fig. 9, the
south pole is _elevated_, the north pole _depressed_, and the diurnal
circles are _oblique_ to the horizon, leaning to the north. When the
diurnal circles are oblique to the horizon, as in Figs. 8 and 9, the
celestial sphere is called an _oblique sphere_.

When the observer is at the equator, as in Fig. 10, the poles of the
heavens are on the horizon, and the diurnal circles are _perpendicular_
to the horizon.

When the observer is at one of the poles, as in Fig. 11, the poles of
the heavens are in the zenith and the nadir, and the diurnal circles are
_parallel_ with the horizon.

[Illustration: Fig. 10.]

[Illustration: Fig. 11.]

6. _Elevation of the Pole and of the Equinoctial._--At the equator the
poles of the heavens lie on the horizon, and the celestial equator
passes through the zenith. As a person moves north from the equator, his
zenith moves north from the celestial equator, and his horizon moves
down from the north pole, and up from the south pole. The distance of
the zenith from the equinoctial, and of the horizon from the celestial
poles, will always be equal to the distance of the observer from the
equator. In other words, the elevation of the pole is equal to the
latitude of the place. In Fig. 12, _O_ is the point of observation, _Z_
the zenith, and _SN_ the horizon. _NP_, the elevation of the pole, is
equal to _ZE_, the distance of the zenith from the equinoctial, and to
the distance of _O_ from the equator, or the latitude of the place.

Two angles, or two arcs, which together equal 90°, are said to be
_complements_ of each other. _ZE_ and _ES_ in Fig. 12 are together equal
to 90°: hence they are complements of each other. _ZE_ is equal to the
latitude of the place, and _ES_ is the _elevation_ of the equinoctial
above the horizon: hence the elevation of the equinoctial is equal to
the complement of the latitude of the place.

[Illustration: Fig. 12.]

Were the observer south of the equator, the zenith would be south of the
equinoctial, and the south pole of the heavens would be the elevated
pole.

[Illustration: Fig. 13.]

_7. Four Sets of Stars._--At most points of observation there are four
sets of stars. These four sets are shown in Fig. 13.

(1) The stars in the neighborhood of the elevated pole _never set_. It
will be seen from Fig. 13, that if the distance of a star from the
elevated pole does not exceed the elevation of the pole, or the latitude
of the place, its diurnal circle will be wholly above the horizon. As
the observer approaches the equator, the elevation of the pole becomes
less and less, and the belt of circumpolar stars becomes narrower and
narrower: at the equator it disappears entirely. As the observer
approaches the pole, the elevation of the pole increases, and the belt
of circumpolar stars becomes broader and broader, until at the pole it
includes half of the heavens. At the poles, no stars rise or set, and
only half of the stars are ever seen at all.

(2) The stars in the neighborhood of the depressed pole _never rise_.
The breadth of this belt also increases as the observer approaches the
pole, and decreases as he approaches the equator, to vanish entirely
when he reaches the equator. The distance from the depressed pole to the
margin of this belt is always equal to the latitude of the place.

(3) The stars in the neighborhood of the equinoctial, on the side of the
elevated pole, _set, but are above the horizon longer than they are
below it_. This belt of stars extends from the equinoctial to a point
whose distance from the elevated pole is equal to the latitude of the
place: in other words, the breadth of this third belt of stars is equal
to the complement of the latitude of the place. Hence this belt of stars
becomes broader and broader as the observer approaches the equator, and
narrower and narrower as he approaches the pole. However, as the
observer approaches the equator, the horizon comes nearer and nearer the
celestial axis, and the time a star is below the horizon becomes more
nearly equal to the time it is above it. As the observer approaches the
pole, the horizon moves farther and farther from the axis, and the time
any star of this belt is below the horizon becomes more and more unequal
to the time it is above it. The farther any star of this belt is from
the equinoctial, the longer the time it is above the horizon, and the
shorter the time it is below it.

(4) The stars which are in the neighborhood of the equinoctial, on the
side of the depressed pole, _rise, but are below the horizon longer than
they are above it_. The width of this belt is also equal to the
complement of the latitude of the place. The farther any star of this
belt is from the equinoctial, the longer time it is below the horizon,
and the shorter time it is above it; and, the farther the place from the
equator, the longer every star of this belt is below the horizon, and
the shorter the time it is above it.

At the equator every star is above the horizon just half of the time;
and any star on the equinoctial is above the horizon just half of the
time in every part of the earth, since the equinoctial and horizon,
being great circles, bisect each other.

8. _Vertical Circles._--Great circles perpendicular to the horizon are
called _vertical circles_. All vertical circles pass through the zenith
and nadir. A number of these circles are shown in Fig. 14, in which
_SENW_ represents the horizon, and _Z_ the zenith.

[Illustration: Fig. 14.]

The vertical circle which passes through the north and south points of
the horizon is called the _meridian_; and the one which passes through
the east and west points, the _prime vertical_. These two circles are
shown in Fig. 15; _SZN_ being the meridian, and _EZW_ the prime
vertical. These two circles are at right angles to each other, or 90°
apart; and consequently they divide the horizon into four quadrants.

[Illustration: Fig. 15.]

9. _Altitude and Zenith Distance._--The _altitude_ of a heavenly body is
its distance above the horizon, and its _zenith distance_ is its
distance from the zenith. Both the altitude and the zenith distance of a
body are measured on the vertical circle which passes through the body.
The altitude and zenith distance of a heavenly body are complements of
each other.

10. _Azimuth and Amplitude.--Azimuth_ is distance measured east or west
from the meridian. When a heavenly body lies north of the prime
vertical, its azimuth is measured from the meridian on the north; and,
when it lies south of the prime vertical, its azimuth is measured from
the meridian on the south. The azimuth of a body can, therefore, never
exceed 90°. The azimuth of a body is the angle which the plane of the
vertical circle passing through it makes with that of the meridian.

The _amplitude_ of a body is its distance measured north or south from
the prime vertical. The amplitude and azimuth of a body are complements
of each other.

11. _Alt-azimuth Instrument._--An instrument for measuring the altitude
and azimuth of a heavenly body is called an _alt-azimuth_ instrument.
One form of this instrument is shown in Fig. 16. It consists essentially
of a telescope mounted on a vertical circle, and capable of turning on a
horizontal axis, which, in turn, is mounted on the vertical axis of a
horizontal circle. Both the horizontal and the vertical circles are
graduated, and the horizontal circle is placed exactly parallel with the
plane of the horizon.

When the instrument is properly adjusted, the axis of the telescope will
describe a vertical circle when the telescope is turned on the
horizontal axis, no matter to what part of the heavens it has been
pointed.

The horizontal and vertical axes carry each a pointer. These pointers
move over the graduated circles, and mark how far each axis turns.

To find the _azimuth_ of a star, the instrument is turned on its
vertical axis till its vertical circle is brought into the plane of the
meridian, and the reading of the horizontal circle noted. The telescope
is then directed to the star by turning it on both its vertical and
horizontal axes. The reading of the horizontal circle is again noted.
The difference between these two readings of the horizontal circle will
be the azimuth of the star.

[Illustration: Fig. 16.]

To find the _altitude_ of a star, the reading of the vertical circle is
first ascertained when the telescope is pointed horizontally, and again
when the telescope is pointed at the star. The difference between these
two readings of the vertical circle will be the altitude of the star.

12. _The Vernier._--To enable the observer to read the fractions of the
divisions on the circles, a device called a _vernier_ is often employed.
It consists of a short, graduated arc, attached to the end of an arm _c_
(Fig. 17), which is carried by the axis, and turns with the telescope.
This arc is of the length of _nine_ divisions on the circle, and it is
divided into _ten_ equal parts. If 0 of the vernier coincides with any
division, say 6, of the circle, 1 of the vernier will be 1/10 of a
division to the left of 7, 2 will be 2/10 of a division to the left of
8, 3 will be 3/10, of a division to the left of 9, etc. Hence, when 1
coincides with 7, 0 will be at 6-1/10; when 2 coincides with 8, 0 will
be at 6-2/10; when 3 coincides with 9, 0 will be at 6-3/10, etc.

[Illustration: Fig. 17.]

To ascertain the reading of the circle by means of the vernier, we first
notice the zero line. If it exactly coincides with any division of the
circle, the number of that division will be the reading of the circle.
If there is not an exact coincidence of the zero line with any division
of the circle, we run the eye along the vernier, and note which of its
divisions does coincide with a division of the circle. The reading of
the circle will then be the number of the first division on the circle
behind the 0 of the vernier, and a number of tenths equal to the number
of the division of the vernier, which coincides with a division of the
circle. For instance, suppose 0 of the vernier beyond 6 of the circle,
and 7 of the vernier to coincide with 13 of the circle. The reading of
the circle will then be 6-7/10.

13. _Hour Circles._--Great circles perpendicular to the celestial
equator are called _hour circles_. These circles all pass through the
poles of the heavens, as shown in Fig. 18. _EQ_ is the celestial
equator, and _P_ and _P'_ are the poles of the heavens.

The point _A_ on the equinoctial (Fig. 19) is called the _vernal
equinox_, or the _first point of Aries_. The hour circle, _APP'_, which
passes through it, is called the _equinoctial colure_.

[Illustration: Fig. 18.]

14. _Declination and Right Ascension._--The _declination_ of a heavenly
body is its distance north or south of the celestial equator. The _polar
distance_ of a heavenly body is its distance from the nearer pole.
Declination and polar distance are measured on hour circles, and for the
same heavenly body they are complements of each other.

[Illustration: Fig. 19.]

The _right ascension_ of a heavenly body is its distance eastward from
the first point of Aries, measured from the equinoctial colure. It is
equal to the arc of the celestial equator included between the first
point of Aries and the hour circle which passes through the heavenly
body. As right ascension is measured eastward entirely around the
celestial sphere, it may have any value from 0° up to 360°. Right
ascension corresponds to longitude on the earth, and declination to
latitude.

15. _The Meridian Circle._--The right ascension and declination of a
heavenly body are ascertained by means of an instrument called the
_meridian circle_, or _transit instrument_. A side-view of this
instrument is shown in Fig. 20.

[Illustration: Fig. 20.]

It consists essentially of a telescope mounted between two piers, so as
to turn in the plane of the meridian, and carrying a graduated circle.
The readings of this circle are ascertained by means of fixed
microscopes, under which it turns. A heavenly body can be observed with
this instrument, only when it is crossing the meridian. For this reason
it is often called the _transit circle_.

To find the declination of a star with this instrument, we first
ascertain the reading of the circle when the telescope is pointed to the
pole, and then the reading of the circle when pointed to the star on its
passage across the meridian. The difference between these two readings
will be the polar distance of the star, and the complement of them the
declination of the star.

To ascertain the reading of the circle when the telescope is pointed to
the pole, we must select one of the circumpolar stars near the pole, and
then point the telescope to it when it crosses the meridian, both above
and below the pole, and note the reading of the circle in each case. The
mean of these two readings will be the reading of the circle when the
telescope is pointed to the pole.

16. _Astronomical Clock._--An _astronomical clock_, or _sidereal clock_
as it is often called, is a clock arranged so as to mark hours from 1 to
24, instead of from 1 to 12, as in the case of an ordinary clock, and so
adjusted as to mark 0 when the vernal equinox, or first point of Aries,
is on the meridian.

As the first point of Aries makes a complete circuit of the heavens in
twenty-four hours, it must move at the rate of 15° an hour, or of 1° in
four minutes: hence, when the astronomical clock marks 1, the first
point of Aries must be 15° west of the meridian, and when it marks 2,
30° west of the meridian, etc. That is to say, by observing an accurate
astronomical clock, one can always tell how far the meridian at any time
is from the first point of Aries.

17. _How to find Right Ascension with the Meridian Circle._--To find the
right ascension of a heavenly body, we have merely to ascertain the
exact time, by the astronomical clock, at which the body crosses the
meridian. If a star crosses the meridian at 1 hour 20 minutes by the
astronomical clock, its right ascension must be 19°; if at 20 hours, its
right ascension must be 300°.

To enable the observer to ascertain with great exactness the time at
which a star crosses the meridian, a number of equidistant and parallel
spider-lines are stretched across the focus of the telescope, as shown
in Fig. 21. The observer notes the time when the star crosses each
spider-line; and the mean of all of these times will be the time when
the star crosses the meridian. The mean of several observations is
likely to be more nearly exact than any single observation.

[Illustration: Fig. 21.]

[Illustration: Fig. 22.]

18. _The Equatorial Telescope._--The _equatorial_ telescope is mounted
on two axes,--one parallel with the axis of the earth, and the other at
right angles to this, and therefore parallel with the plane of the
earth's equator. The former is called the _polar axis_, and the latter
the _declination axis_. Each axis carries a graduated circle. These
circles are called respectively the _hour circle_ and the _declination
circle_. The telescope is attached directly to the declination axis.
When the telescope is fixed in any declination, and then turned on its
polar axis, the line of sight will describe a diurnal circle; so that,
when the tube is once directed to a star, it can be made to follow the
star by simply turning the telescope on its polar axis.

In the case of large instruments of this class, the polar axis is
usually turned by clock-work at the rate at which the heavens rotate; so
that, when the telescope has once been pointed to a planet or other
heavenly body, it will continue to follow the body and keep it steadily
in the field of view without further trouble on the part of the
observer.

The great Washington Equatorial is shown in Fig. 22. Its object-glass is
26 inches in diameter, and its focal length is 32-1/2 feet. It was
constructed by Alvan Clark & Sons of Cambridge, Mass. It is one of the
three largest refracting telescopes at present in use. The Newall
refractor at Gateshead, Eng., has an objective 25 inches in diameter,
and a focal length of 29 feet. The great refractor at Vienna has an
objective 27 inches in diameter. There are several large refractors now
in process of construction.

[Illustration: Fig. 23.]

19. _The Wire Micrometer._--Large arcs in the heavens are measured by
means of the graduated circles attached to the axes of the telescopes;
but small arcs within the field of view of the telescope are measured by
means of instruments called _micrometers_, mounted in the focus of the
telescope. One of the most convenient of these micrometers is that known
as the _wire micrometer_, and shown in Fig. 23.

The frame _AA_ covers two slides, _C_ and _D_. These slides are moved by
the screws _F_ and _G_. The wires _E_ and _B_ are stretched across the
ends of the slides so as to be parallel to each other. On turning the
screws _F_ and _G_ one way, these wires are carried apart; and on
turning them the other way they are brought together again. Sometimes
two parallel wires, _x_ and _y_, shown in the diagram at the right, are
stretched across the frame at right angles to the wires _E_, _B_. We may
call the wires _x_ and _y_ the _longitudinal_ wires of the micrometer,
and _E_ and _B_ the _transverse_ wires. Many instruments have only one
longitudinal wire, which is stretched across the middle of the focus.
The longitudinal wires are just in front of the transverse wires, but do
not touch them.

To find the distance between any two points in the field of view with a
micrometer, with a single longitudinal wire, turn the frame till the
longitudinal wire passes through the two points; then set the wires _E_
and _B_ one on each point, turn one of the screws, known as the
_micrometer screw_, till the two wires are brought together, and note
the number of times the screw is turned. Having previously ascertained
over what arc one turn of the screw will move the wire, the number of
turns will enable us to find the length of the arc between the two
points.

The threads of the micrometer screw are cut with great accuracy; and the
screw is provided with a large head, which is divided into a hundred or
more equal parts.

These divisions, by means of a fixed pointer, enable us to ascertain
what fraction of a turn the screw has made over and above its complete
revolutions.

20. _Reflecting Telescopes._--It is possible to construct mirrors of
much larger size than lenses: hence reflecting telescopes have an
advantage over refracting telescopes as regards size of aperture and of
light-gathering power. They are, however, inferior as regards
definition; and, in order to prevent flexure, it is necessary to give
the speculum, or mirror, a massiveness which makes the telescope
unwieldy. It is also necessary frequently to repolish the speculum; and
this is an operation of great delicacy, as the slightest change in the
form of the surface impairs the definition of the image. These defects
have been remedied, to a certain extent, by the introduction of
silver-on-glass mirrors; that is, glass mirrors covered in front with a
thin coating of silver. Glass is only one-third as heavy as
speculum-metal, and silver is much superior to that metal in reflecting
power; and when the silver becomes tarnished, it can be removed and
renewed without danger of changing the form of the glass.

_The Herschelian Reflector._--In this form of telescope the mirror is
slightly tipped, so that the image, instead of being formed in the
centre of the tube, is formed near one side of it, as in Fig. 24. The
observer can then view it without putting his head inside the tube, and
therefore without cutting off any material portion of the light. In
observation, he must stand at the upper or outer end of the tube, and
look into it, his back being turned towards the object. From his looking
directly into the mirror, it is also sometimes called the _front-view_
telescope. The great disadvantage of this arrangement is, that the rays
cannot be brought to an exact focus when they are thrown so far to one
side of the axis, and the injury to the definition is so great that the
front-view plan is now entirely abandoned.

[Illustration: Fig. 24.]

_The Newtonian Reflector._--The plan proposed by Sir Isaac Newton was to
place a small plane mirror just inside the focus, inclined to the
telescope at an angle of 45°, so as to throw the rays to the side of the
tube, where they come to a focus, and form the image. An opening is made
in the side of the tube, just below where the image is formed; and in
this opening the eye-piece is inserted. The small mirror cuts off some
of the light, but not enough to be a serious defect. An improvement
which lessens this defect has been made by Professor Henry Draper. The
inclined mirror is replaced by a small rectangular prism (Fig. 25), by
reflection from which the image is formed very near the prism. A pair of
lenses are then inserted in the course of the rays, by which a second
image is formed at the opening in the side of the tube; and this second
image is viewed by an ordinary eye-piece.

[Illustration: Fig. 25.]

_The Gregorian Reflector._--This is a form proposed by James Gregory,
who probably preceded Newton as an inventor of the reflecting telescope.
Behind the focus, _F_ (Fig. 26), a small concave mirror, _R_, is placed,
by which the light is reflected back again down the tube. The larger
mirror, _M_, has an opening through its centre; and the small mirror,
_R_, is so adjusted as to form a second image of the object in this
opening. This image is then viewed by an eye-piece which is screwed into
the opening.

[Illustration: Fig. 26.]

_The Cassegrainian Reflector._--In principle this is the same with the
Gregorian; but the small mirror, _R_, is convex, and is placed inside
the focus, _F_, so that the rays are reflected from it before reaching
the focus, and no image is formed until they reach the opening in the
large mirror. This form has an advantage over the Gregorian, in that the
telescope may be made shorter, and the small mirror can be more easily
shaped to the required figure. It has, therefore, entirely superseded
the original Gregorian form.

[Illustration: Fig. 27.]

Optically these forms of telescope are inferior to the Newtonian; but
the latter is subject to the inconvenience, that the observer must be
stationed at the upper end of the telescope, where he looks into an
eye-piece screwed into the side of the tube.

On the other hand, the Cassegrainian Telescope is pointed directly at
the object to be viewed, like a refractor; and the observer stands at
the lower end, and looks in at the opening through the large mirror.
This is, therefore, the most convenient form of all in management.

[Illustration: Fig. 28.]

The largest reflecting telescope yet constructed is that of Lord Rosse,
at Parsonstown, Ireland. Its speculum is 6 feet in diameter, and its
focal length 55 feet. It is commonly used as a Newtonian. This telescope
is shown in Fig. 27.

The great telescope of the Melbourne Observatory, Australia, is a
Cassegranian reflector. Its speculum is 4 feet in diameter, and its
focal length is 32 feet. It is shown in Fig. 28.

[Illustration: Fig. 29.]

The great reflector of the Paris Observatory is a Newtonian reflector.
Its mirror of silvered glass is 4 feet in diameter, and its focal length
is 23 feet. This telescope is shown in Fig. 29.

21. _The Sun's Motion among the Stars._--If we notice the stars at the
same hour night after night, we shall find that the constellations are
steadily advancing towards the west. New constellations are continually
appearing in the east, and old ones disappearing in the west. This
continual advancing of the heavens towards the west is due to the fact
that the sun's place among the stars is _continually moving towards the
east_. The sun completes the circuit of the heavens in a year, and is
therefore moving eastward at the rate of about a degree a day.

[Illustration: Fig. 30.]

This motion of the sun's place among the stars is due to the revolution
of the earth around the sun, and not to any real motion of the sun. In
Fig. 30 suppose the inner circle to represent the orbit of the earth
around the sun, and the outer circle to represent the celestial sphere.
When the earth is at _E_, the sun's place on the celestial sphere is at
_S'_. As the earth moves in the direction _EF_, the sun's place on the
celestial sphere must move in the direction _S'T_: hence the revolution
of the earth around the sun would cause the sun's place among the stars
to move around the heavens in the same direction that the earth is
moving around the sun.

22. _The Ecliptic._--The circle described by the sun in its apparent
motion around the heavens is called the _ecliptic_. The plane of this
circle passes through the centre of the earth, and therefore through the
centre of the celestial sphere; the earth being so small, compared with
the celestial sphere, that it practically makes no difference whether we
consider a point on its surface, or one at its centre, as the centre of
the celestial sphere. The ecliptic is, therefore, a great circle.

The earth's orbit lies in the plane of the ecliptic; but it extends only
an inappreciable distance from the sun towards the celestial sphere.

[Illustration: Fig. 31.]

23. _The Obliquity of the Ecliptic._--The ecliptic is inclined to the
celestial equator by an angle of about 23-1/2°. This inclination is
called the _obliquity of the ecliptic_. The obliquity of the ecliptic is
due to the deviation of the earth's axis from a perpendicular to the
plane of its orbit. The axis of a rotating body tends to maintain the
same direction; and, as the earth revolves around the sun, its axis
points all the time in nearly the same direction. The earth's axis
deviates about 23-1/2° from the perpendicular to its orbit; and, as the
earth's equator is at right angles to its axis, it will deviate about
23-1/2° from the plane of the ecliptic. The celestial equator has the
same direction as the terrestrial equator, since the axis of the heavens
has the same direction as the axis of the earth.

[Illustration: Fig. 32.]

Suppose the globe at the centre of the tub (Fig. 31) to represent the
sun, and the smaller globes to represent the earth in various positions
in its orbit. The surface of the water will then represent the plane of
the ecliptic, and the rod projecting from the top of the earth will
represent the earth's axis, which is seen to point all the time in the
same direction, or to lean the same way. The leaning of the axis from
the perpendicular to the surface of the water would cause the earth's
equator to be inclined the same amount to the surface of the water, half
of the equator being above, and half of it below, the surface. Were the
axis of the earth perpendicular to the surface of the water, the earth's
equator would coincide with the surface, as is evident from Fig. 32.

[Illustration: Fig. 33.]

24. _The Equinoxes and Solstices._--The ecliptic and celestial equator,
being great circles, bisect each other. Half of the ecliptic is north,
and half of it is south, of the equator. The points at which the two
circles cross are called the _equinoxes_. The one at which the sun
crosses the equator from south to north is called the _vernal_ equinox,
and the one at which it crosses from north to south the _autumnal_
equinox. The points on the ecliptic midway between the equinoxes are
called the _solstices_. The one north of the equator is called the
_summer_ solstice, and the one south of the equator the _winter_
solstice. In Fig. 33, _EQ_ is the celestial equator, _EcE'c'_ the
ecliptic, _V_ the vernal equinox, A the autumnal equinox, Ec the winter
solstice, and _E'c'_ the summer solstice.

[Illustration: Fig. 34.]

25. _The Inclination of the Ecliptic to the Horizon._--Since the
celestial equator is perpendicular to the axis of the heavens, it makes
the same angle with it on every side: hence, at any place, the equator
makes always the same angle with the horizon, whatever part of it is
above the horizon. But, as the ecliptic is oblique to the equator, it
makes different angles with the celestial axis on different sides; and
hence, at any place, the angle which the ecliptic makes with the horizon
varies according to the part which is above the horizon. The two extreme
angles for a place more than 23-1/2° north of the equator are shown in
Figs. 34 and 35.

The least angle is formed when the vernal equinox is on the eastern
horizon, the autumnal on the western horizon, and the winter solstice on
the meridian, as in Fig. 34. The angle which the ecliptic then makes
with the horizon is equal to the elevation of the equinoctial _minus_
23-1/2°. In the latitude of New York this angle = 49° - 23-1/2° =
25-1/2°.

[Illustration: Fig. 35.]

The greatest angle is formed when the autumnal equinox is on the eastern
horizon, the vernal on the western horizon, and the summer solstice is
on the meridian (Fig. 35). The angle between the ecliptic and the
horizon is then equal to the elevation of the equinoctial _plus_
23-1/2°. In the latitude of New York this angle = 49° + 23-1/2° =
72-1/2°.

Of course the equinoxes, the solstices, and all other points on the
ecliptic, describe diurnal circles, like every other point in the
heavens: hence, in our latitude, these points rise and set every day.

26. _Celestial Latitude and Longitude._--_Celestial latitude_ is
distance measured north or south from the ecliptic; and _celestial
longitude_ is distance measured on the ecliptic eastward from the vernal
equinox, or the first point of Aries. Great circles perpendicular to the
ecliptic are called _celestial meridians_. These circles all pass
through the poles of the ecliptic, which are some 23-1/2° from the poles
of the equinoctial. The latitude of a heavenly body is measured by the
arc of a celestial meridian included between the body and the ecliptic.
The longitude of a heavenly body is measured by the arc of the ecliptic
included between the first point of Aries and the meridian which passes
through the body. There are, of course, always two arcs included between
the first point of Aries and the meridian,--one on the east, and the
other on the west, of the first point of Aries. The one on the _east_ is
always taken as the measure of the longitude.

27. _The Precession of the Equinoxes._--The equinoctial points have a
slow westward motion along the ecliptic. This motion is at the rate of
about 50'' a year, and would cause the equinoxes to make a complete
circuit of the heavens in a period of about twenty-six thousand years.
It is called the _precession of the equinoxes_. This westward motion of
the equinoxes is due to the fact that the axis of the earth has a slow
gyratory motion, like the handle of a spinning-top which has begun to
wabble a little. This gyratory motion causes the axis of the heavens to
describe a cone in about twenty-six thousand years, and the pole of the
heavens to describe a circle about the pole of the ecliptic in the same
time. The radius of this circle is 23-1/2°.

[Illustration: Fig. 36.]

    28. _Illustration of Precession._--The precession of the equinoxes
    may be illustrated by means of the apparatus shown in Fig. 36. The
    horizontal and stationary ring _EC_ represents the ecliptic; the
    oblique ring _E'Q_ represents the equator; _V_ and _A_ represent the
    equinoctial point, and _E_ and _C_ the solstitial points; _B_
    represents the pole of the ecliptic, _P_ the pole of the equator,
    and _PO_ the celestial axis. The ring _E'Q_ is supported on a pivot
    at _O_; and the rod _BP_, which connects _B_ and _P_, is jointed at
    each end so as to admit of the movement of _P_ and _B_.

    On carrying _P_ around _B_, we shall see that _E'Q_ will always
    preserve the same obliquity to _EC_, and that the points _V_ and _A_
    will move around the circle _EC_. The same will also be true of the
    points _E_ and _C_.

29. _Effects of Precession._--One effect of precession, as has already
been stated, is the revolution of the pole of the heavens around the
pole of the ecliptic in a period of about twenty-six thousand years. The
circle described by the pole of the heavens, and the position of the
pole at various dates, are shown in Fig. 37, where o indicates the
position of the pole at the birth of Christ. The numbers round the
circle to the left of o are dates A.D., and those to the right of o are
dates B.C. It will be seen that the star at the end of the Little Bear's
tail, which is now near the north pole, will be exactly at the pole
about the year 2000. It will then recede farther and farther from the
pole till the year 15000 A.D., when it will be about forty-seven degrees
away from the pole. It will be noticed that one of the stars of the
Dragon was the pole star about 2800 years B.C. There are reasons to
suppose that this was about the time of the building of the Great
Pyramid.

A second effect of precession is the shifting of the signs along the
zodiac. The _zodiac_ is a belt of the heavens along the ecliptic,
extending eight degrees from it on each side. This belt is occupied by
twelve constellations, known as the _zodiacal constellations_. They are
_Aries_, _Taurus_, _Gemini_, _Cancer_, _Leo_, _Virgo_, _Libra_,
_Scorpio_, _Sagittarius_, _Capricornus_, _Aquarius_, and _Pisces_. The
zodiac is also divided into twelve equal parts of thirty degrees each,
called _signs_. These signs have the same names as the twelve zodiacal
constellations, and when they were first named, each sign occupied the
same part of the zodiac as the corresponding constellation; that is to
say, the sign Aries was in the constellation Aries, and the sign Taurus
in the constellation Taurus, etc. Now the signs are always reckoned as
beginning at the vernal equinox, which is continually shifting along the
ecliptic; so that the signs are continually moving along the zodiac,
while the constellations remain stationary: hence it has come about that
the _first point of Aries_ (the _sign_) is no longer in the
_constellation_ Aries, but in Pisces.

[Illustration: Fig. 37.]

Fig. 38 shows the position of the vernal equinox 2170 B.C. It was then
in Taurus, just south of the Pleiades. It has since moved from Taurus,
through Aries, and into Pisces, as shown in Fig. 39.

[Illustration: Fig. 38.]

[Illustration: Fig. 39.]

Since celestial longitude and right ascension are both measured from the
first point of Aries, the longitude and right ascension of the stars are
slowly changing from year to year. It will be seen, from Figs. 38 and
39, that the declination is also slowly changing.

30. _Nutation._--The gyratory motion of the earth's axis is not
perfectly regular and uniform. The earth's axis has a slight tremulous
motion, oscillating to and fro through a short distance once in about
nineteen years. This tremulous motion of the axis causes the pole of the
heavens to describe an undulating curve, as shown in Fig. 40, and gives
a slight unevenness to the motion of the equinoxes along the ecliptic.
This nodding motion of the axis is called _nutation_.

[Illustration: Fig. 40.]

31. _Refraction._--When a ray of light from one of the heavenly bodies
enters the earth's atmosphere obliquely, it will be bent towards a
perpendicular to the surface of the atmosphere, since it will be
entering a denser medium. As the ray traverses the atmosphere, it will
be continually passing into denser and denser layers, and will therefore
be bent more and more towards the perpendicular. This bending of the ray
is shown in Fig. 41. A ray which started from _A_ would enter the eye at
_C_, as if it came from _I_: hence a star at _A_ would appear to be at
_I_.

[Illustration: Fig. 41.]

Atmospheric refraction displaces all the heavenly bodies from the
horizon towards the zenith. This is evident from Fig. 42. _OD_ is the
horizon, and _Z_ the zenith, of an observer at _O_. Refraction would
make a star at _Q_ appear at _P_: in other words, it would displace it
towards the zenith. A star in the zenith is not displaced by refraction,
since the rays which reach the eye from it traverse the atmosphere
vertically. The farther a star is from the zenith, the more it is
displaced by refraction, since the greater is the obliquity with which
the rays from it enter the atmosphere.

[Illustration: Fig. 42.]

At the horizon the displacement by refraction is about half a degree;
but it varies considerably with the state of the atmosphere. Refraction
causes a heavenly body to appear above the horizon longer than it really
is above it, since it makes it appear to be on the horizon when it is
really half a degree below it.

The increase of refraction towards the horizon often makes the sun, when
near the horizon, appear distorted, the lower limb of the sun being
raised more than the upper limb. This distortion is shown in Fig. 43.
The vertical diameter of the sun appears to be considerably less than
the horizontal diameter.

[Illustration: Fig. 43.]

32. _Parallax._--_Parallax_ is the displacement of an object caused by a
change in the point of view from which it is seen. Thus in Fig. 44, the
top of the tower _S_ would be seen projected against the sky at _a_ by
an observer at _A_, and at _b_ by an observer at _B_. In passing from
_A_ to _B_, the top of the tower is displaced from _a_ to _b_, or by the
angle _aSb_. This angle is called the parallax of _S_, as seen from _B_
instead of _A_.

[Illustration: Fig. 44.]

The _geocentric parallax_ of a heavenly body is its displacement caused
by its being seen from the surface of the earth, instead of from the
centre of the earth. In Fig. 45, _R_ is the centre of the earth, and _O_
the point of observation on the surface of the earth. Stars at _S_,
_S'_, and _S''_, would, from the centre of the earth, appear at _Q_,
_Q'_, and _Q''_; while from the point _O_ on the surface of the earth,
these same stars would appear at _P_, _P'_ and _P''_, being displaced
from their position, as seen from the centre of the earth, by the angles
_QSP_, _Q'S'P'_, and _Q''S''P''_. It will be seen that parallax
displaces a body from the zenith towards the horizon, and that the
parallax of a body is greatest when it is on the horizon. The parallax
of a heavenly body when on the horizon is called its _horizontal
parallax_. A body in the zenith is not displaced by parallax, since it
would be seen in the same direction from both the centre and the surface
of the earth.

[Illustration: Fig. 45.]

The parallax of a body at _S'''_ is _Q'''S'''P_, which is seen to be
greater than _QSP_; that is to say, the parallax of a heavenly body
increases with its nearness to the earth. The distance and parallax of a
body are so related, that, either being known, the other may be
computed.

    33. _Aberration._--_Aberration_ is a slight displacement of a star,
    owing to an apparent change in the direction of the rays of light
    which proceed from it, caused by the motion of the earth in its
    orbit. If we walk rapidly in any direction in the rain, when the
    drops are falling vertically, they will appear to come into our
    faces from the direction in which we are walking. Our own motion has
    apparently changed the direction in which the drops are falling.

    [Illustration: Fig. 46.]

    In Fig. 46 let _A_ be a gun of a battery, from which a shot is fired
    at a ship, _DE_, that is passing. Let _ABC_ be the course of the
    shot. The shot enters the ship's side at _B_, and passes out at the
    other side at _C_; but in the mean time the ship has moved from _E_
    to _e_, and the part _B_, where the shot entered, has been carried
    to _b_. If a person on board the ship could see the ball as it
    crossed the ship, he would see it cross in the diagonal line _bC_;
    and he would at once say that the cannon was in the direction of
    _Cb_. If the ship were moving in the opposite direction, he would
    say that the cannon was just as far the other side of its true
    position.

    Now, we see a star in the direction in which the light coming from
    the star appears to be moving. When we examine a star with a
    telescope, we are in the same condition as the person who on
    shipboard saw the cannon-ball cross the ship. The telescope is
    carried along by the earth at the rate of eighteen miles a second:
    hence the light will appear to pass through the tube in a slightly
    different direction from that in which it is really moving: just as
    the cannon-ball appears to pass through the ship in a different
    direction from that in which it is really moving. Thus in Fig. 47, a
    ray of light coming in the direction _SOT_ would appear to traverse
    the tube _OT_ of a telescope, moving in the direction of the arrow,
    as if it were coming in the direction _S'O_.

[Illustration: Fig. 47.]

    As light moves with enormous velocity, it passes through the tube so
    quickly, that it is apparently changed from its true direction only
    by a very slight angle: but it is sufficient to displace the star.
    This apparent change in the direction of light caused by the motion
    of the earth is called _aberration of light_.

34. _The Planets._--On watching the stars attentively night after night,
it will be found, that while the majority of them appear _fixed_ on the
surface of the celestial sphere, so as to maintain their relative
positions, there are a few that _wander_ about among the stars,
alternately advancing towards the east, halting, and retrograding
towards the west. These wandering stars are called _planets_.

Their motions appear quite irregular; but, on the whole, their eastward
motion is in excess of their westward, and in a longer or shorter time
they all complete the circuit of the heavens. In almost every instance,
their paths are found to lie wholly in the belt of the zodiac.

[Illustration: Fig. 48.]

Fig. 48 shows a portion of the apparent path of one of the planets.

                                  II.
                           THE SOLAR SYSTEM.


                     I. THEORY OF THE SOLAR SYSTEM.


35. _Members of the Solar System._--The solar system is composed of the
_sun_, _planets_, _moons_, _comets_, and _meteors_. Five planets,
besides the earth, are readily distinguished by the naked eye, and were
known to the ancients: these are _Mercury_, _Venus_, _Mars_, _Jupiter_,
and _Saturn_. These, with the _sun_ and _moon_, made up the _seven
planets_ of the ancients, from which the seven days of the week were
named.


                         The Ptolemaic System.


36. _The Crystalline Spheres._--We have seen that all the heavenly
bodies appear to be situated on the surface of the celestial sphere. The
ancients assumed that the stars were really fixed on the surface of a
crystalline sphere, and that they were carried around the earth daily by
the rotation of this sphere. They had, however, learned to distinguish
the planets from the stars, and they had come to the conclusion that
some of the planets were nearer the earth than others, and that all of
them were nearer the earth than the stars are. This led them to imagine
that the heavens were composed of a number of crystalline spheres, one
above another, each carrying one of the planets, and all revolving
around the earth from east to west, but at different rates. This
structure of the heavens is shown in section in Fig. 49.

[Illustration: Fig. 49.]

37. _Cycles and Epicycles._--The ancients had also noticed that, while
all the planets move around the heavens from west to east, their motion
is not one of uniform advancement. Mercury and Venus appear to oscillate
to and fro across the sun, while Jupiter and Saturn appear to oscillate
to and fro across a centre which is moving around the earth, so as to
describe a series of loops, as shown in Fig. 50.

[Illustration: Fig. 50.]

The ancients assumed that the planets moved in exact circles, and, in
fact, that all motion in the heavens was circular, the circle being the
simplest and most perfect curve. To account for the loops described by
the planets, they imagined that each planet revolved in a circle around
a centre, which, in turn, revolved in a circle around the earth. The
circle described by this centre around the earth they called the
_cycle_, and the circle described by the planet around this centre they
called the _epicycle_.

38. _The Eccentric._--The ancients assumed that the planets moved at a
uniform rate in describing the epicycle, and also the centre in
describing the cycle. They had, however, discovered that the planets
advance eastward more rapidly in some parts of their orbits than in
others. To account for this they assumed that the cycles described by
the centre, around which the planets revolved, were _eccentric_; that is
to say, that the earth was not at the centre of the cycle, but some
distance away from it, as shown in Fig. 51. _E_ is the position of the
earth, and _C_ is the centre of the cycle. The lines from _E_ are drawn
so as to intercept equal arcs of the cycle. It will be seen at once that
the angle between any pair of lines is greatest at _P_, and least at
_A_; so that, were a planet moving at the same rate at _P_ and _A_, it
would seem to be moving much faster at _P_. The point _P_ of the
planet's cycle was called its _perigee_, and the point A its _apogee_.

[Illustration: Fig. 51.]

As the apparent motion of the planets became more accurately known, it
was found necessary to make the system of cycles, epicycles, and
eccentrics exceedingly complicated to represent that motion.


                         The Copernican System.


39. _Copernicus._--Copernicus simplified the Ptolemaic system greatly by
assuming that the earth and all the planets revolved about the sun as a
centre. He, however, still maintained that all motion in the heavens was
circular, and hence he could not rid his system entirely of cycles and
epicycles.


                         Tycho Brahe's System.


40. _Tycho Brahe._--Tycho Brahe was the greatest of the early
astronomical observers. He, however, rejected the system of Copernicus,
and adopted one of his own, which was much more complicated. He held
that all the planets but the earth revolved around the sun, while the
sun and moon revolved around the earth. This system is shown in Fig. 52.

[Illustration: Fig. 52.]


                            Kepler's System.


41. _Kepler._--While Tycho Brahe devoted his life to the observation of
the planets. Kepler gave his to the study of Tycho's observations, for
the purpose of discovering the true laws of planetary motion. He
banished the complicated system of cycles, epicycles, and eccentrics
forever from the heavens, and discovered the three laws of planetary
motion which have rendered his name immortal.

42. _The Ellipse._--An _ellipse_ is a closed curve which has two points
within it, the sum of whose distances from every point on the curve is
the same. These two points are called the _foci_ of the ellipse.

[Illustration: Fig. 53.]

One method of describing an ellipse is shown in Fig. 53. Two tacks, _F_
and _F'_, are stuck into a piece of paper, and to these are fastened the
two ends of a string which is longer than the distance between the
tacks. A pencil is then placed against the string, and carried around,
as shown in the figure. The curve described by the pencil is an ellipse.
The two points _F_ and _F'_ are the foci of the ellipse: the sum of the
distances of these two points from every point on the curve is equal to
the length of the string. When half of the ellipse has been described,
the pencil must be held against the other side of the string in the same
way, and carried around as before.

The point _O_, half way between _F_ and _F'_, is called the _centre_ of
the ellipse; _AA'_ is the _major axis_ of the ellipse, and _CD_ is the
_minor axis_.

43. _The Eccentricity of the Ellipse._--The ratio of the distance
between the two foci to the major axis of the ellipse is called the
_eccentricity_ of the ellipse. The greater the distance between the two
foci, compared with the major axis of the ellipse, the greater is the
eccentricity of the ellipse; and the less the distance between the foci,
compared with the length of the major axis, the less the eccentricity of
the ellipse. The ellipse of Fig. 54 has an eccentricity of 1/8. This
ellipse scarcely differs in appearance from a circle. The ellipse of
Fig. 55 has an eccentricity of 1/2, and that of Fig. 56 an eccentricity
of 7/8.

[Illustration: Fig. 54.]

[Illustration: Fig. 55.]

[Illustration: Fig. 56.]

44. _Kepler's First Law._--Kepler first discovered that _all the planets
move from west to east in ellipses which have the sun as a common
focus_. This law of planetary motion is known as _Kepler's First Law_.
The planets appear to describe loops, because we view them from a moving
point.

The ellipses described by the planets differ in eccentricity; and,
though they all have one focus at the sun, their major axes have
different directions. The eccentricity of the planetary orbits is
comparatively small. The ellipse of Fig. 54 has seven times the
eccentricity of the earth's orbit, and twice that of the orbit of any of
the larger planets except Mercury; and its eccentricity is more than
half of that of the orbit of Mercury. Owing to their small eccentricity,
the orbits of the planets are usually represented by circles in
astronomical diagrams.

[Illustration: Fig. 57.]

45. _Kepler's Second Law._--Kepler next discovered that a planet's rate
of motion in the various parts of its orbit is such that _a line drawn
from the planet to the sun would always sweep over equal areas in equal
times_. Thus, in Fig. 57, suppose the planet would move from _P_ to
_P^1_ in the same time that it would move from _P^2_ to _P^3_, or from
_P^4_ to _P^5_; then the dark spaces, which would be swept over by a
line joining the sun and the planet, in these equal times, would all be
equal.

A line drawn from the sun to a planet is called the _radius vector_ of
the planet. The radius vector of a planet is shortest when the planet is
nearest the sun, or at _perihelion_, and longest when the planet is
farthest from the sun, or at _aphelion_: hence, in order to have the
areas equal, it follows that a planet must move fastest when at
perihelion, and slowest at aphelion.

_Kepler's Second Law_ of planetary motion is usually stated as follows:
_The radius vector of a planet describes equal areas in equal times in
every part of the planet's orbit_.

46. _Kepler's Third Law._--Kepler finally discovered that the periodic
times of the planets bear the following relation to the distances of the
planets from the sun: _The squares of the periodic times of the planets
are to each other as the cubes of their mean distances from the sun_.
This is known as _Kepler's Third Law_ of planetary motion. By _periodic
time_ is meant the time it takes a planet to revolve around the sun.

These three laws of Kepler's are the foundation of modern physical
astronomy.


                         The Newtonian System.


47. _Newton's Discovery._--Newton followed Kepler, and by means of his
three laws of planetary motion made his own immortal discovery of the
_law of gravitation_. This law is as follows: _Every portion of matter
in the universe attracts every other portion with a force varying
directly as the product of the masses acted upon, and inversely as the
square of the distances between them._

48. _The Conic Sections._--The _conic sections_ are the figures formed
by the various plane sections of a right cone. There are four classes of
figures formed by these sections, according to the angle which the plane
of the section makes with the axis of the cone.

_OPQ_, Fig. 58, is a right cone, and _ON_ is its axis. Any section,
_AB_, of this cone, whose plane is perpendicular to the axis of the
cone, is a _circle_.

[Illustration: Fig. 58.]

Any section, _CD_, of this cone, whose plane is oblique to the axis, but
forms with it an angle greater than _NOP_, is an _ellipse_. The less the
angle which the plane of the section makes with the axis, the more
elongated is the ellipse.

Any section, _EF_, of this cone, whose plane makes with the axis an
angle equal to _NOP_, is a _parabola_. It will be seen, that, by
changing the obliquity of the plane _CD_ to the axis _NO_, we may pass
uninterruptedly from the circle through ellipses of greater and greater
elongation to the parabola.

Any section, _GH_, of this cone, whose plane makes with the axis _ON_ an
angle less than _NOP_, is a _hyperbola_.

[Illustration: Fig. 59.]

It will be seen from Fig. 59, in which comparative views of the four
conic sections are given, that the circle and the ellipse are _closed_
curves, or curves which return into themselves. The parabola and the
hyperbola are, on the contrary, _open_ curves, or curves which do not
return into themselves.

    49. _A Revolving Body is continually Falling towards its Centre of
    Revolution._--In Fig. 60 let _M_ represent the moon, and _E_ the
    earth around which the moon is revolving in the direction _MN_. It
    will be seen that the moon, in moving from M to N, falls towards the
    earth a distance equal to _mN_. It is kept from falling into the
    earth by its orbital motion.

[Illustration: Fig. 60.]

    The fact that a body might be projected forward fast enough to keep
    it from falling into the earth is evident from Fig. 61. _AB_
    represents the level surface of the ocean, _C_ a mountain from the
    summit of which a cannon-ball is supposed to be fired in the
    direction _CE_. _AD_ is a line parallel with _CE_; _DB_ is a line
    equal to the distance between the two parallel lines _AD_ and _CE_.
    This distance is equal to that over which gravity would pull a ball
    towards the centre of the earth in a minute. No matter, then, with
    what velocity the ball _C_ is fired, at the end of a minute it will
    be somewhere on the line _AD_. Suppose it were fired fast enough to
    reach the point _D_ in a minute: it would be on the line _AD_ at the
    end of the minute, but still just as far from the surface of the
    water as when it started. It will be seen, that, although it has all
    the while been falling towards the earth, it has all the while kept
    at exactly the same distance from the surface. The same thing would
    of course be true during each succeeding minute, till the ball came
    round to _C_ again, and the ball would continue to revolve in a
    circle around the earth.

[Illustration: Fig. 61.]

50. _The Form of a Body's Orbit depends upon the Rate of its Forward
Motion._--If the ball _C_ were fired fast enough to reach the line _AD_
beyond the point _D_, it would be farther from the surface at the end of
the second than when it started. Its orbit would no longer be circular,
but _elliptical_. If the speed of projection were gradually augmented,
the orbit would become a more and more elongated ellipse. At a certain
rate of projection, the orbit would become a _parabola_; at a still
greater rate, a _hyperbola_.

51. _The Moon held in her Orbit by Gravity._--Newton compared the
distance _mN_ that the moon is drawn to the earth in a given time, with
the distance a body near the surface of the earth would be pulled toward
the earth in the same time; and he found that these distances are to
each other inversely as the squares of the distances of the two bodies
from the centre of the earth. He therefore concluded that _the moon is
drawn to the earth by gravity_, and that the _intensity of gravity
decreases as the square of the distance increases_.

[Illustration: Fig. 62.]

52. _Any Body whose Orbit is a Conic Section, and which moves according
to Kepler's Second Law, is acted upon by a Force varying inversely as
the Square of the Distance._--Newton compared the distance which any
body, moving in an ellipse, according to Kepler's Second Law, is drawn
towards the sun in the same time in different parts of its orbit. He
found these distances in all cases to vary inversely as the square of
the distance of the planet from the sun. Thus, in Fig. 62, suppose a
planet would move from _K_ to _B_ in the same time that it would move
from _k_ to _b_ in another part of its orbit. In the first instance the
planet would be drawn towards the sun the distance _AB_, and in the
second instance the distance _ab_. Newton found that _AB : ab = (SK)^2 :
(Sk)^2_. He also found that the same would be true when the body moved
in a parabola or a hyperbola: hence he concluded that _every body that
moves around the sun in an ellipse, a parabola, or a hyperbola, is
moving under the influence of gravity_.

[Transcriber's Note: In Newton's equation above, (SK)^2 means to group S
and K together and square their product. In the original book, instead
of using parentheses, there was a vinculum, a horizontal bar, drawn over
the S and the K to express the same grouping.]

[Illustration: Fig. 63.]

53. _The Force that draws the Different Planets to the Sun Varies
inversely as the Squares of the Distances of the Planets from the
Sun._--Newton compared the distances _jK_ and _eF_, over which two
planets are drawn towards the sun in the same time, and found these
distances to vary inversely as the squares of the distances of the
planets from the sun: hence he concluded that _all the planets are held
in their orbits by gravity_. He also showed that this would be true of
any two bodies that were revolving around the sun's centre, according to
Kepler's Third Law.

54. _The Copernican System._--The theory of the solar system which
originated with Copernicus, and which was developed and completed by
Kepler and Newton, is commonly known as the _Copernican System_. This
system is shown in Fig. 64.

[Illustration: Fig. 64.]


                        II. THE SUN AND PLANETS.


                             I. THE EARTH.


                             Form and Size.


55. _Form of the Earth._--In ordinary language the term _horizon_
denotes the line that bounds the portion of the earth's surface that is
visible at any point.

(1) It is well known that the horizon of a plain presents the form of a
circle surrounding the observer. If the latter moves, the circle moves
also; but its form remains the same, and is modified only when mountains
or other obstacles limit the view. Out at sea, the circular form of the
horizon is still more decided, and changes only near the coasts, the
outline of which breaks the regularity.

Here, then, we obtain a first notion of the rotundity of the earth,
since a sphere is the only body which is presented always to us under
the form of a circle, from whatever point on its surface it is viewed.

(2) Moreover, it cannot be maintained that the horizon is the vanishing
point of distinct vision, and that it is this which causes the
appearance of a circular boundary, because the horizon is enlarged when
we mount above the surface of the plain. This will be evident from Fig.
65, in which a mountain is depicted in the middle of a plain, whose
uniform curvature is that of a sphere. From the foot of the mountain the
spectator will have but a very limited horizon. Let him ascend half way,
his visual radius extends, is inclined below the first horizon, and
reveals a more extended circular area. At the summit of the mountain the
horizon still increases; and, if the atmosphere is pure, the spectator
will see numerous objects where from the lower stations the sky alone
was visible.

[Illustration: Fig. 65.]

This extension of the horizon would be inexplicable if the earth had the
form of an extended plane.

(3) The curvature of the surface of the sea manifests itself in a still
more striking manner. If we are on the coast at the summit of a hill,
and a vessel appears on the horizon (Fig. 66), we see only the tops of
the masts and the highest sails; the lower sails and the hull are
invisible. As the vessel approaches, its lower part comes into view
above the horizon, and soon it appears entire.

[Illustration: Fig. 66.]

In the same manner the sailors from the ship see the different parts of
objects on the land appear successively, beginning with the highest. The
reason of this will be evident from Fig. 67, where the course of a
vessel, seen in profile, is figured on the convex surface of the sea.

[Illustration: Fig. 67.]

As the curvature of the ocean is the same in every direction, it follows
that the surface of the ocean is _spherical_. The same is true of the
surface of the land, allowance being made for the various inequalities
of the surface. From these and various other indications, we conclude
that _the earth is a sphere_.

56. _Size of the Earth._--The size of the earth is ascertained by
measuring the length of a degree of a meridian, and multiplying this by
three hundred and sixty. This gives the circumference of the earth as
about twenty-five thousand miles, and its diameter as about eight
thousand miles. We know that the two stations between which we measure
are one degree apart when the elevation of the pole at one station is
one degree greater than at the other.

57. _The Earth Flattened at the Poles._--Degrees on the meridian have
been measured in various parts of the earth, and it has been found that
they invariably increase in length as we proceed from the equator
towards the pole: hence the earth must curve less and less rapidly as we
approach the poles; for the less the curvature of a circle, the larger
the degrees on it.

[Illustration: Fig. 68.]

58. _The Earth in Space._--In Fig. 68 we have a view of the earth
suspended in space. The side of the earth turned towards the sun is
illumined, and the other side is in darkness. As the planet rotates on
its axis, successive portions of it will be turned towards the sun. As
viewed from a point in space between it and the sun, it will present
light and dark portions, which will assume different forms according to
the portion which is illumined. These different appearances are shown in
Fig. 69.

[Illustration: Fig. 69.]


                             Day and Night.


59. _Day and Night._--The succession of day and night is due to _the
rotation of the earth on its axis_, by which a place on the surface of
the earth is carried alternately into the sunshine and out of it. As the
sun moves around the heavens on the ecliptic, it will be on the
celestial equator when at the equinoxes, and 23-1/2° north of the
equator when at the summer solstice, and 23-1/2° south of the equator
when at the winter solstice.

60. _Day and Night when the Sun is at the Equinoxes._--When the sun is
at either equinox, the diurnal circle described by the sun will coincide
with the celestial equator; and therefore half of this diurnal circle
will be above the horizon at every point on the surface of the globe. At
these times _day and night will be equal in every part of the earth_.

[Illustration: Fig. 70.]

[Illustration: Fig. 71.]

    The equality of days and nights when the sun is on the celestial
    equator is also evident from the following considerations: one-half
    of the earth is in sunshine all of the time; when the sun is on the
    celestial equator, it is directly over the equator of the earth, and
    the illumination extends from pole to pole, as is evident from Figs.
    70 and 71, in the former of which the sun is represented as on the
    eastern horizon at a place along the central line of the figure, and
    in the latter as on the meridian along the same line. In each
    diagram it is seen that the illumination extends from pole to pole:
    hence, as the earth rotates on its axis, every place on the surface
    will be in the sunshine and out of it just half of the time.

61. _Day and Night when the Sun is at the Summer Solstice._--When the
sun is at the summer solstice, it will be 23-1/2° north of the celestial
equator. The diurnal circle described by the sun will then be 23-1/2°
north of the celestial equator; and more than half of this diurnal
circle will be above the horizon at all places north of the equator, and
less than half of it at places south of the equator: hence _the days
will be longer than the nights at places north of the equator, and
shorter than the nights at places south of the equator_. At places
within 23-1/2° of the north pole, the entire diurnal circle described by
the sun will be above the horizon, so that the sun will not set. At
places within 23-1/2° of the south pole of the earth, the entire diurnal
circle will be below the horizon, so that the sun will not rise.

[Illustration: Fig. 72.]

[Illustration: Fig. 73.]

    The illumination of the earth at this time is shown in Figs. 72 and
    73. In Fig. 72 the sun is represented as on the western horizon
    along the middle line of the figure, and in Fig. 73 as on the
    meridian. It is seen at once that the illumination extends 23-1/2°
    beyond the north pole, and falls 23-1/2° short of the south pole. As
    the earth rotates on its axis, places near the north pole will be in
    the sunshine all the time, while places near the south pole will be
    out of the sunshine all the time. All places north of the equator
    will be in the sunshine longer than they are out of it, while all
    places south of the equator will be out of the sunshine longer than
    they are in it.

62. _Day and Night when the Sun is at the Winter Solstice._--When the
sun is at the winter solstice, it is 23-1/2° south of the celestial
equator. The diurnal circle described by the sun is then 23-1/2° south
of the celestial equator. More than half of this diurnal circle will
therefore be above the horizon at all places south of the equator, and
less than half of it at all places north of the equator: hence _the days
will be longer than the nights south of the equator, and shorter than
the nights at places north of the equator_. At places within 23-1/2° of
the south pole, the diurnal circle described by the sun will be entirely
above the horizon, and the sun will therefore not set. At places within
23-1/2° of the north pole, the diurnal circle described by the sun will
be wholly below the horizon, and therefore the sun will not rise.

    The illumination of the earth at this time is shown in Figs. 74 and
    75, and is seen to be the reverse of that shown in Figs. 72 and 73.

[Illustration: Fig. 74.]

[Illustration: Fig. 75.]

63. _Variation in the Length of Day and Night._--As long as the sun is
north of the equinoctial, the nights will be longer than the days south
of the equator, and shorter than the days north of the equator. It is
just the reverse when the sun is south of the equator.

The farther the sun is from the equator, the greater is the inequality
of the days and nights.

The farther the place is from the equator, the greater the inequality of
its days and nights.

When the distance of a place from the _north_ pole is less than the
distance of the sun north of the equinoctial, it will have _continuous
day without night_, since the whole of the sun's diurnal circle will be
above the horizon. A place within the same distance of the _south_ pole
will have _continuous night_.

When the distance of a place from the _north_ pole is less than the
distance of the sun south of the equinoctial, it will have _continuous
night_, since the whole of the sun's diurnal circle will then be below
the horizon. A place within the same distance of the _south_ pole will
then have _continuous day_.

At the _equator_ the _days and nights are always equal_; since, no
matter where the sun is in the heavens, half of all the diurnal circles
described by it will be above the horizon, and half of them below it.

64. _The Zones._--It will be seen, from what has been stated above, that
the sun will at some time during the year be directly overhead at every
place within 23-1/2° of the equator on either side. This belt of the
earth is called the _torrid zone_. The torrid zone is bounded by circles
called the _tropics_; that of _Cancer_ on the north, and that of
_Capricorn_ on the south.

It will also be seen, that, at every place within 23-1/2° of either
pole, there will be, some time during the year, a day during which the
sun will not rise, or on which it will not set. These two belts of the
earth's surface are called the _frigid zones_. These zones are bounded
by the _arctic_ circles. The nearer a place is to the poles, the greater
the number of days on which the sun does not rise or set.

Between the frigid zones and the torrid zones, there are two belts on
the earth which are called the _temperate zones_. The sun is never
overhead at any place in these two zones, but it rises and sets every
day at every place within their limits.

65. _The Width of the Zones._--The distance the frigid zones extend from
the poles, and the torrid zones from the equator, is exactly equal to
_the obliquity of the ecliptic_, or the deviation of the axis of the
earth from the perpendicular to the plane of its orbit. Were this
deviation forty-five degrees, the obliquity of the ecliptic would be
forty-five degrees, the torrid zone would extend forty-five degrees from
the equator, and the frigid zones forty-five degrees from the poles. In
this case there would be no temperate zones. Were this deviation fifty
degrees, the torrid and frigid zones would overlap ten degrees, and
there would be two belts of ten degrees on the earth, which would
experience alternately during the year a torrid and a frigid climate.

Were the axis of the earth perpendicular to the plane of the earth's
orbit, there would be no zones on the earth, and no variation in the
length of day and night.

66. _Twilight._--Were it not for the atmosphere, the darkness of
midnight would begin the moment the sun sank below the horizon, and
would continue till he rose again above the horizon in the east, when
the darkness of the night would be suddenly succeeded by the full light
of day. The gradual transition from the light of day to the darkness of
the night, and from the darkness of the night to the light of day, is
called _twilight_, and is due to the _diffusion of light from the upper
layers of the atmosphere_ after the sun has ceased to shine on the lower
layers at night, or before it has begun to shine on them in the morning.

[Illustration: Fig. 76.]

Let _ABCD_ (Fig. 76) represent a portion of the earth, _A_ a point on
its surface where the sun _S_ is setting; and let _SAH_ be a ray of
light just grazing the earth at _A_, and leaving the atmosphere at the
point _H_. The point _A_ is illuminated by the whole reflective
atmosphere _HGFE_. The point _B_, to which the sun has set, receives no
direct solar light, nor any reflected from that part of the atmosphere
which is below _ALH_; but it receives a twilight from the portion _HLF_,
which lies above the visible horizon _BF_. The point _C_ receives a
twilight only from the small portion of the atmosphere; while at _D_ the
twilight has ceased altogether.

67. _Duration of Twilight._--The astronomical limit of twilight is
generally understood to be the instant when stars of the sixth magnitude
begin to be visible in the zenith at evening, or disappear in the
morning.

    Twilight is usually reckoned to last until the sun's depression
    below the horizon amounts to eighteen degrees: this, however,
    varies; in the tropics a depression of sixteen or seventeen degrees
    being sufficient to put an end to the phenomenon, while in England a
    depression of seventeen to twenty-one degrees is required. The
    duration of twilight differs in different latitudes; it varies also
    in the same latitude at different seasons of the year, and depends,
    in some measure, on the meteorological condition of the atmosphere.
    When the sky is of a pale color, indicating the presence of an
    unusual amount of condensed vapor, twilight is of longer duration.
    This happens habitually in the polar regions. On the contrary,
    within the tropics, where the air is pure and dry, twilight
    sometimes lasts only fifteen minutes. Strictly speaking, in the
    latitude of Greenwich there is no true night from May 22 to July 21,
    but constant twilight from sunset to sunrise. Twilight reaches its
    minimum three weeks before the vernal equinox, and three weeks after
    the autumnal equinox, when its duration is an hour and fifty
    minutes. At midwinter it is longer by about seventeen minutes; but
    the augmentation is frequently not perceptible, owing to the greater
    prevalence of clouds and haze at that season of the year, which
    intercept the light, and hinder it from reaching the earth. The
    duration is least at the equator (an hour and twelve minutes), and
    increases as we approach the poles; for at the former there are two
    twilights every twenty-four hours, but at the latter only two in a
    year, each lasting about fifty days. At the north pole the sun is
    below the horizon for six months, but from Jan. 29 to the vernal
    equinox, and from the autumnal equinox to Nov. 12, the sun is less
    than eighteen degrees below the horizon; so that there is twilight
    during the whole of these intervals, and thus the length of the
    actual night is reduced to two months and a half. The length of the
    day in these regions is about six months, during the whole of which
    time the sun is constantly above the horizon. The general rule is,
    _that to the inhabitants of an oblique sphere the twilight is longer
    in proportion as the place is nearer the elevated pole, and the sun
    is farther from the equator on the side of the elevated pole_.


                              The Seasons.


68. _The Seasons._--While the sun is north of the celestial equator,
places north of the equator are receiving heat from the sun by day
longer than they are losing it by radiation at night, while places south
of the equator are losing heat by radiation at night longer than they
are receiving it from the sun by day. When, therefore, the sun passes
north of the equator, the temperature begins to rise at places north of
the equator, and to fall at places south of it. The rise of temperature
is most rapid north of the equator when the sun is at the summer
solstice; but, for some time after this, the earth continues to receive
more heat by day than it loses by night, and therefore the temperature
continues to rise. For this reason, the heat is more excessive after the
sun passes the summer solstice than before it reaches it.

69. _The Duration of the Seasons._--Summer is counted as beginning in
June, when the sun is at the summer solstice, and as continuing until
the sun reaches the autumnal equinox, in September. Autumn then begins,
and continues until the sun is at the winter solstice, in December.
Winter follows, continuing until the sun comes to the vernal equinox, in
March, when spring begins, and continues to the summer solstice. In
popular reckoning the seasons begin with the first day of June,
September, December, and March.

The reason why winter is counted as occurring after the winter solstice
is similar to the reason why the summer is placed after the summer
solstice. The earth north of the equator is losing heat most rapidly at
the time of the winter solstice; but for some time after this it loses
more heat by night than it receives by day: hence for some time the
temperature continues to fall, and the cold is more intense after the
winter solstice than before it.

[Illustration: Fig. 77.]

Of course, when it is summer in the northern hemisphere, it is winter in
the southern hemisphere, and the reverse. Fig. 77 shows the portion of
the earth's orbit included in each season. It will be seen that the
earth is at perihelion in the winter season for places north of the
equator, and at aphelion in the summer season. This tends to mitigate
somewhat the extreme temperatures of our winters and summers.

[Illustration: Fig. 78.]

70. _The Illumination of the Earth at the different Seasons._--Fig. 78
shows the earth as it would appear to an observer at the sun during each
of the four seasons; that is to say, the portion of the earth that is
receiving the sun's rays. Figs. 79, 80, 81, and 82 are enlarged views of
the earth, as seen from the sun at the time of the summer solstice, of
the autumnal equinox, of the winter solstice, and of the vernal equinox.

[Illustration: Fig. 79.]

[Illustration: Fig. 80.]

[Illustration: Fig. 81.]

[Illustration: Fig. 82.]

[Illustration: Fig. 83.]

Fig. 83 is, so to speak, a side view of the earth, showing the limit of
sunshine on the earth when the sun is at the summer solstice; and Fig.
84, showing the limit of sunshine when the sun is at the autumnal
equinox.

[Illustration: Fig. 84.]

71. _Cause of the Change of Seasons._--Variety in the length of day and
night, and diversity in the seasons, depend upon _the obliquity of the
ecliptic_. Were there no obliquity of the ecliptic, there would be no
inequality in the length of day and night, and but slight diversity of
seasons. The greater the obliquity of the ecliptic, the greater would be
the variation in the length of the days and nights, and the more extreme
the changes of the seasons.


                                 Tides.


72. _Tides._--The alternate rise and fall of the surface of the sea
twice in the course of a lunar day, or of twenty-four hours and
fifty-one minutes, is known as the _tides_. When the water is rising, it
is said to be _flood_ tide; and when it is falling, _ebb_ tide. When the
water is at its greatest height, it is said to be _high_ water; and when
at its least height, _low_ water.

    73. _Cause of the Tides._--It has been known to seafaring nations
    from a remote antiquity that there is a singular connection between
    the ebb and flow of the tides and the diurnal motion of the moon.

[Illustration: Fig. 85.]

    This tidal movement in seeming obedience to the moon was a mystery
    until the study of the law of gravitation showed it to be due to
    _the attraction of the moon on the waters of the ocean_. The reason
    why there are two tides a day will appear from Fig. 85. Let _M_ be
    the moon, _E_ the earth, and _EM_ the line joining their centres.
    Now, strictly speaking, the moon does not revolve around the earth
    any more than the earth around the moon; but the centre of each body
    moves around the common centre of gravity of the two bodies. The
    earth being eighty times as heavy as the moon, this centre is
    situated within the former, about three-quarters of the way from its
    centre to its surface, at the point _G_. The body of the earth
    itself being solid, every part of it, in consequence of the moon's
    attraction, may be considered as describing a circle once in a
    month, with a radius equal to _EG_. The centrifugal force caused by
    this rotation is just balanced by the mean attraction of the moon
    upon the earth. If this attraction were the same on every part of
    the earth, there would be everywhere an exact balance between it and
    the centrifugal force. But as we pass from _E_ to _D_ the attraction
    of the moon diminishes, owing to the increased distance: hence at
    _D_ the centrifugal force predominates, and the water therefore
    tends to move away from the centre _E_. As we pass from _E_ towards
    _C_, the attraction of the moon increases, and therefore exceeds the
    centrifugal force: consequently at _C_ there is a tendency to draw
    the water towards the moon, but still away from the centre _E_. At
    _A_ and _B_ the attraction of the moon increases the gravity of the
    water, owing to the convergence of the lines _BM_ and _AM_, along
    which it acts: hence the action of the moon tends to make the waters
    rise at _D_ and _C_, and to fall at _A_ and _B_, causing two tides
    to each apparent diurnal revolution of the moon.

    74. _The Lagging of the Tides._--If the waters everywhere yielded
    immediately to the attractive force of the moon, it would always be
    high water when the moon was on the meridian, low water when she was
    rising or setting, and high water again when she was on the meridian
    below the horizon. But, owing to the inertia of the water, some time
    is necessary for so slight a force to set it in motion; and, once in
    motion, it continues so after the force has ceased, and until it has
    acted some time in the opposite direction. Therefore, if the motion
    of the water were unimpeded, it would not be high water until some
    hours after the moon had passed the meridian. The free motion of the
    water is also impeded by the islands and continents. These deflect
    the tidal wave from its course in such a way that it may, in some
    cases, be many hours, or even a whole day, behind its time.
    Sometimes two waves meet each other, and raise a very high tide. In
    some places the tides run up a long bay, where the motion of a large
    mass of water will cause an enormous tide to be raised. In the Bay
    of Fundy both of these causes are combined. A tidal wave coming up
    the Atlantic coast meets the ocean wave from the east, and, entering
    the bay with their combined force, they raise the water at the head
    of it to the height of sixty or seventy feet.

75. _Spring-Tides and Neap-Tides._--The sun produces a tide as well as
the moon; but the tide-producing force of the sun is only about
four-tenths of that of the moon. At new and full moon the two bodies
unite their forces, the ebb and flow become greater than the average,
and we have the _spring-tides_. When the moon is in her first or third
quarter, the two forces act against each other; the tide-producing force
is the difference of the two; the ebb and flow are less than the
average; and we have the _neap-tides_.

[Illustration: Fig. 86.]

[Illustration: Fig. 87.]

[Illustration: Fig. 88.]

Fig. 86 shows the tide that would be produced by the moon alone; Fig.
87, the tide produced by the combined action of the sun and moon; and
Fig. 88, by the sun and moon acting at right angles to each other.

The tide is affected by the distance of the moon from the earth, being
highest near the time when the moon is in perigee, and lowest near the
time when she is in apogee. When the moon is in perigee, at or near the
time of a new or full moon, unusually high tides occur.

    76. _Diurnal Inequality of Tides._--The height of the tide at a
    given place is influenced by the declination of the moon. When the
    moon has no declination, the highest tides should occur along the
    equator, and the heights should diminish from thence toward the
    north and south; but the two daily tides at any place should have
    the same height. When the moon has north declination, as shown in
    Fig. 89, the highest tides on the side of the earth next the moon
    will be at places having a corresponding north latitude, as at _B_,
    and on the opposite side at those which have an equal south
    latitude. Of the two daily tides at any place, that which occurs
    when the moon is nearest the zenith should be the greatest: hence,
    when the moon's declination is north, the height of the tide at a
    place in north latitude should be greater when the moon is above the
    horizon than when she is below it. At the same time, places south of
    the equator have the highest tides when the moon is below the
    horizon, and the least when she is above it. This is called the
    _diurnal inequality_, because its cycle is one day; but it varies
    greatly in amount at different places.

[Illustration: Fig. 89.]

77. _Height of Tides._--At small islands in mid-ocean the tides never
rise to a great height, sometimes even less than one foot; and the
average height of the tides for the islands of the Atlantic and Pacific
Oceans is only three feet and a half. Upon approaching an extensive
coast where the water is shallow, the height of the tide is increased;
so that, while in mid-ocean the average height does not exceed three
feet and a half, the average in the neighborhood of continents is not
less than four or five feet.


                           The Day and Time.


78. _The Day._--By the term _day_ we sometimes denote the period of
sunshine as contrasted with that of the absence of sunshine, which we
call _night_, and sometimes the period of the earth's rotation on its
axis. It is with the latter signification that the term is used in this
section. As the earth rotates on its axis, it carries the meridian of a
place with it; so that, during each complete rotation of the earth, the
portion of the meridian which passes overhead from pole to pole sweeps
past every star in the heavens from west to east. The _interval between
two successive passages of this portion of the meridian across the same
star_ is the exact period of the complete rotation of the earth. This
period is called a _sidereal day_. The sidereal day may also be defined
as _the interval between two successive passages of the same star across
the meridian_; the passage of the meridian across the star, and the
passage or _transit_ of the star across the meridian, being the same
thing looked at from a different point of view. The interval _between
two successive passages of the meridian across the sun_, or _of the sun
across the meridian_, is called a _solar day_.

79. _Length of the Solar Day._--The solar day is a little longer than
the sidereal day. This is owing to the sun's eastward motion among the
stars. We have already seen that the sun's apparent position among the
stars is continually shifting towards the east at a rate which causes it
to make a complete circuit of the heavens in a year, or three hundred
and sixty-five days. This is at the rate of about one degree a day:
hence, were the sun and a star on the meridian together to-day, when the
meridian again came around to the star, the sun would appear about one
degree to the eastward: hence the meridian must be carried about one
degree farther in order to come up to the sun. The solar day must
therefore be _about four minutes longer_ than the sidereal day.

[Illustration: Fig. 90.]

[Illustration: Fig. 91.]

The fact that the earth must make more than a complete rotation is also
evident from Figs. 90 and 91. In Fig. 90, _ba_ represents the plane of
the meridian, and the small arrows indicate the direction the earth is
rotating on its axis, and revolving in its orbit. When the earth is at
1, the sun is on the meridian at _a_. When the earth has moved to 2, it
has made a complete rotation, as is shown by the fact that the plane of
the meridian is parallel with its position at 1; but it is evident that
the meridian has not yet come up with the sun. In Fig. 91, _OA_
represents the plane of the meridian, and _OS_ the direction of the sun.
The small arrows indicate the direction of the rotation and revolution
of the earth. In passing from the first position to the second the earth
makes a complete rotation, but the meridian is not brought up to the
sun.

80. _Inequality in the Length of Solar Days._--The sidereal days are all
of the same length; but the solar days differ somewhat in length. This
difference is due to the fact that the sun's apparent position moves
eastward, or _away from the meridian_, at a variable rate.

    There are three reasons why this rate is variable:--

    (1) The sun's eastward motion is due to the revolution of the earth
    in its orbit. Now, the earth's orbital motion is _not uniform_,
    being fastest when the earth is at perihelion, and slowest when the
    earth is at aphelion: hence, other things being equal, solar days
    will be longest when the earth is at perihelion, and shortest when
    the earth is at aphelion.

[Illustration: Fig. 92.]

[Illustration: Fig. 93.]

    (2) The sun's eastward motion is along the ecliptic. Now, from Figs.
    92 and 93, it will be seen, that, when the sun is at one of the
    equinoxes, it will be moving away from the meridian _obliquely_;
    and, from Figs. 94 and 95, that, when the sun is at one of the
    solstices, it will be moving away from the meridian
    _perpendicularly_: hence, other things being equal, the sun would
    move away from the meridian _fastest_, and the days be _longest_,
    when the sun is at the _solstices_; while it would move away from
    the meridian _slowest_, and the days be _shortest_, when the sun is
    at the _equinoxes_. That a body moving along the ecliptic must be
    moving at a variable angle to the meridian becomes very evident on
    turning a celestial globe so as to bring each portion of the
    ecliptic under the meridian in turn.

[Illustration: Fig. 94.]

[Illustration: Fig. 95.]

    (3) The sun, moving along the ecliptic, always moves _in a great
    circle_, while the point of the meridian which is to overtake the
    sun moves in a diurnal circle, which is _sometimes a great circle_
    and _sometimes a small circle_. When the sun is at the equinoxes,
    the point of the meridian which is to overtake it moves in a great
    circle. As the sun passes from the equinoxes to the solstices, the
    point of the meridian which is to overtake it moves on a smaller and
    smaller circle: hence, as we pass away from the celestial equator,
    the points of the meridian move slower and slower. Therefore, other
    things being equal, the meridian will gain upon the sun _most
    rapidly_, and the days be _shortest_, when the sun is at the
    _equinoxes_; while it will gain on the sun _least rapidly_, and the
    days will be _longest_, when the sun is at the _solstices_.

The ordinary or _civil day_ is the mean of all the solar days in a year.

81. _Sun Time and Clock Time._--It is noon by the sun when the sun is on
the meridian, and by the clock at the middle of the civil day. Now, as
the civil days are all of the same length, while solar days are of
variable length, it seldom happens that the middles of these two days
coincide, or that sun time and clock time agree. The difference between
sun time and clock time, or what is often called _apparent solar time_
and _mean solar time_, is called the _equation of time_. The sun is said
to be _slow_ when it crosses the meridian after noon by the clock, and
_fast_ when it crosses the meridian before noon by the clock. Sun time
and clock time coincide four times a year; during two intermediate
seasons the clock time is ahead, and during two it is behind.

                  *       *       *       *       *

The following are the dates of coincidence and of maximum deviation,
which vary but slightly from year to year:--

    February 10      True sun fifteen minutes slow.
    April 15         True sun correct.
    May 14           True sun four minutes fast.
    June 14          True sun correct.
    July 25          True sun six minutes slow.
    August 31        True sun correct.
    November 2       True sun sixteen minutes fast.
    December 24      True sun correct.

One of the effects of the equation of time which is frequently
misunderstood is, that the interval from sunrise until noon, as given in
the almanacs, is not the same as that between noon and sunset. The
forenoon could not be longer or shorter than the afternoon, if by "noon"
we meant the passage of the sun across the meridian; but the noon of our
clocks being sometimes fifteen minutes before or after noon by the sun,
the former may be half an hour nearer to sunrise than to sunset, or
_vice versa_.


                               The Year.


82. _The Year._--The _year_ is the time it takes the earth to revolve
around the sun, or, what amounts to the same thing, _the time it takes
the sun to pass around the ecliptic_.

(1) The time it takes the sun to pass from a star around to the same
star again is called a _sidereal year_. This is, of course, the exact
time it takes the earth to make a complete revolution around the sun.

[Illustration: Fig. 96.]

(2) The time it takes the sun to pass around from the vernal equinox, or
the _first point of Aries_, to the vernal equinox again, is called the
_tropical_ year. This is a little shorter than the sidereal year, owing
to the precession of the equinoxes. This will be evident from Fig. 96.
The circle represents the ecliptic, _S_ the sun, and _E_ the vernal
equinox. The sun moves around the ecliptic _eastward_, as indicated by
the long arrow, while the equinox moves slowly _westward_, as indicated
by the short arrow. The sun will therefore meet the equinox before it
has quite completed the circuit of the heavens. The exact lengths of
these respective years are:--

    Sidereal year   365.25636=365 days  6 hours   9 min   9 sec
    Tropical year   365.24220=365 days  5 hours  48 min  46 sec

Since the recurrence of the seasons depends on the tropical year, the
latter is the one to be used in forming the calendar and for the
purposes of civil life generally. Its true length is eleven minutes and
fourteen seconds less than three hundred and sixty-five days and a
fourth.

It will be seen that the tropical year is about twenty minutes shorter
than the sidereal year.

    (3) The time it takes the earth to pass from its perihelion point
    around to the perihelion point again is called the _anomalistic
    year_. This year is about four minutes longer than the sidereal
    year. This is owing to the fact that the major axis of the earth's
    orbit is slowly moving around to the east at the rate of about ten
    seconds a year. This causes the perihelion point _P_ (Fig. 97) to
    move _eastward_ at that rate, as indicated by the short arrow. The
    earth _E_ is also moving eastward, as indicated by the long arrow.
    Hence the earth, on starting at the perihelion, has to make a little
    more than a complete circuit to reach the perihelion point again.

[Illustration: Fig. 97.]

    83. _The Calendar._--The _solar year_, or the interval between two
    successive passages of the same equinox by the sun, is 365 days, 5
    hours, 48 minutes, 46 seconds. If, then, we reckon only 365 days to
    a common or _civil year_, the sun will come to the equinox 5 hours,
    48 minutes, 46 seconds, or nearly a quarter of a day, later each
    year; so that, if the sun entered Aries on the 20th of March one
    year, he would enter it on the 21st four years after, on the 22d
    eight years after, and so on. Thus in a comparatively short time the
    spring months would come in the winter, and the summer months in the
    spring.

    Among different ancient nations different methods of computing the
    year were in use. Some reckoned it by the revolution of the moon,
    some by that of the sun; but none, so far as we know, made proper
    allowances for deficiencies and excesses. Twelve moons fell short of
    the true year, thirteen exceeded it; 365 days were not enough, 366
    were too many. To prevent the confusion resulting from these errors,
    Julius Cæsar reformed the calendar by making the year consist of 365
    days, 6 hours (which is hence called a _Julian_ year), and made
    every fourth year consist of 366 days. This method of reckoning is
    called _Old Style_.

    But as this made the year somewhat too long, and the error in 1582
    amounted to ten days, Pope Gregory XIII., in order to bring the
    vernal equinox back to the 21st of March again, ordered ten days to
    be struck out of that year, calling the next day after the 4th of
    October the 15th; and, to prevent similar confusion in the future,
    he decreed that three leap-years should be omitted in the course of
    every four hundred years. This way of reckoning time is called _New
    Style_. It was immediately adopted by most of the European nations,
    but was not accepted by the English until the year 1752. The error
    then amounted to eleven days, which were taken from the month of
    September by calling the 3d of that month the 14th. The Old Style is
    still retained by Russia.

    According to the Gregorian calendar, _every year whose number is
    divisible by four_ is a _leap-year_, except, that, _in the case of
    the years whose numbers are exact hundreds, those only are
    leap-years which are divisible by four after cutting off the last
    two figures_. Thus the years 1600, 2000, 2400, etc., are leap-years;
    1700, 1800, 1900, 2100, 2200, etc., are not. The error will not
    amount to a day in over three thousand years.

    84. _The Dominical Letter._--The _dominical letter_ for any year is
    that which we often see placed against Sunday in the almanacs, and
    is always one of the first seven in the alphabet. Since a common
    year consists of 365 days, if this number is divided by seven (the
    number of days in a week), there will be a remainder of one: hence a
    year commonly begins one day later in the week than the preceding
    one did. If a year of 365 days begins on Sunday, the next will begin
    on Monday; if it begins on Thursday, the next will begin on Friday;
    and so on. If Sunday falls on the 1st of January, the _first_ letter
    of the alphabet, or _A_, is the _dominical letter_. If Sunday falls
    on the 7th of January (as it will the next year, unless the first is
    leap-year), the _seventh_ letter, _G_, is the dominical letter. If
    Sunday falls on the 6th of January (as it will the third year,
    unless the first or second is leap-year), the _sixth_ letter, _F_,
    will be the dominical letter. Thus, if there were no leap-years, the
    dominical letters would regularly follow a retrograde order, _G_,
    _F_, _E_, _D_, _C_, _B_, _A_.

    But _leap_-years have 366 days, which, divided by seven, leaves two
    remainder: hence the years following leap-years will begin two days
    later in the week than the leap-years did. To prevent the
    interruption which would hence occur in the order of the dominical
    letters, leap-years have _two_ dominical letters, one indicating
    Sunday till the 29th of February, and the other for the rest of the
    year.

By _Table I._ below, the dominical letter for any year (New Style) for
four thousand years from the beginning of the Christian Era may be
found; and it will be readily seen how the Table could be extended
indefinitely by continuing the centuries at the top in the same order.

To find the dominical letter by this table, _look for the hundreds of
years at the top, and for the years below a hundred, at the left hand_.

Thus the letter for 1882 will be opposite the number 82, and in the
column having 1800 at the top; that is, it will be _A_. In the same way,
the letters for 1884, which is a leap-year, will be found to be _FE_.

Having the dominical letter of any year, _Table II._ shows what days of
every month of the year will be _Sundays_.

To find the Sundays of any month in the year by this table, _look in the
column, under the dominical letter, opposite the name of the month given
at the left_.

From the Sundays the date of any other day of the week can be readily
found.

Thus, if we wish to know on what day of the week Christmas falls in
1889, we look opposite December, under the letter _F_ (which we have
found to be the dominical letter for the year), and find that the 22d of
the month is a Sunday; the 25th, or Christmas, will then be Wednesday.

In the same way we may find the day of the week corresponding to any
date (New Style) in history. For instance, the 17th of June, 1775, the
day of the fight at Bunker Hill, is found to have been a _Saturday_.

These two tables then serve as a _perpetual almanac_.

TABLE I.

                                  100  200  300  400
                                  500  600  700  800
                                  900 1000 1100 1200
                                 1300 1400 1500 1600
                                 1700 1800 1900 2000
                                 2100 2200 2300 2400
                                  ---  ---  --- ----
                                    C    E    G   BA

                     1 29 57 85     B    D    F    G
                     2 30 58 86     A    C    E    F
                     3 31 59 87     G    B    D    E
                     4 32 60 88    FE   AG   CB   DC
                     5 33 61 89     D    F    A    B
                     6 34 62 90     C    E    G    A
                     7 35 63 91     B    D    F    G
                     8 36 64 92    AG   CB   ED   FE
                     9 37 65 93     F    A    C    D
                    10 38 66 94     E    G    B    C
                    11 39 67 95     D    F    A    B
                    12 40 68 96    CB   ED   GF   AG
                    13 41 69 97     A    C    E    F
                    14 42 70 98     G    B    D    E
                    15 43 71 99     F    A    C    D
                    16 44 72 ..    ED   GF   BA   CB
                    17 45 73 ..     C    E    G    A
                    18 46 74 ..     B    D    F    G
                    19 47 75 ..     A    C    E    F
                    20 48 76 ..    GF   BA   DC   ED
                    21 49 77 ..     E    G    B    C
                    22 50 78 ..     D    F    A    B
                    23 51 79 ..     C    E    G    A
                    24 52 80 ..    BA   DC   FE   GF
                    25 53 81 ..     G    B    D    E
                    26 54 82 ..     F    A    C    D
                    27 55 83 ..     E    G    B    C
                    28 56 84 ..    DC   FE   AG   BA

TABLE II.

                                 A  B  C  D  E  F  G

                                 1  2  3  4  5  6  7
                   Jan. 31.      8  9 10 11 12 13 14
                                15 16 17 18 19 20 21
                   Oct. 31.     22 23 24 25 26 27 28
                                29 30 31 .. .. .. ..

                   Feb. 28-29.  .. .. ..  1  2  3  4
                                 5  6  7  8  9 10 11
                   March 31.    12 13 14 15 16 17 18
                                19 20 21 22 23 24 25
                   Nov. 30.     26 27 28 29 30 31 ..

                                .. .. .. .. .. ..  1
                   April 30.     2  3  4  5  6  7  8
                                 9 10 11 12 13 14 15
                   July 31      16 17 18 19 20 21 22
                                23 24 25 26 27 28 29
                                30 31 .. .. .. .. ..

                                .. ..  1  2  3  4  5
                                 6  7  8  9 10 11 12
                   Aug. 31.     13 14 15 16 17 18 19
                                20 21 22 23 24 25 26
                                27 28 29 30 31 .. ..

                                .. .. .. .. ..  1  2
                   Sept. 30.     3  4  5  6  7  8  9
                                10 11 12 13 14 15 16
                                17 18 19 20 21 22 23
                   Dec. 31.     24 25 26 27 28 29 30
                                31 .. .. .. .. .. ..

                                ..  1  2  3  4  5  6
                                 7  8  9 10 11 12 13
                   May. 31.     14 15 16 17 18 19 20
                                21 22 23 24 25 26 27
                                28 29 30 31 .. .. ..

                                .. .. .. ..  1  2  3
                                 4  5  6  7  8  9 10
                   June 30.     11 12 13 14 15 16 17
                                18 19 20 21 22 23 24
                                25 26 27 28 29 30 ..


                  Weight of the Earth and Precession.


85. _The Weight of the Earth._--There are several methods of
ascertaining the weight and mass of the earth. The simplest, and perhaps
the most trustworthy method is to compare the pull of the earth upon a
ball of lead with that of a known mass of lead upon it. The pull of a
known mass of lead upon the ball may be measured by means of a torsion
balance. One form of the balance employed for this purpose is shown in
Figs. 98 and 99. Two small balls of lead, _b_ and _b_, are fastened to
the ends of a light rod _e_, which is suspended from the point _F_ by
means of the thread _FE_. Two large balls of lead, _W_ and _W_, are
placed on a turn-table, so that one of them shall be just in front of
one of the small balls, and the other just behind the other small ball.
The pull of the large balls turns the rod around a little so as to bring
the small balls nearer the large ones. The small balls move towards the
large ones till they are stopped by the torsion of the thread, which is
then equal to the pull of the large balls. The deflection of the rod is
carefully measured. The table is then turned into the position indicated
by the dotted lines in Fig. 99, so as to reverse the position of the
large balls with reference to the small ones. The rod is now deflected
in the opposite direction, and the amount of deflection is again
carefully measured. The second measurement is made as a check upon the
accuracy of the first. The force required to twist the thread as much as
it was twisted by the deflection of the rod is ascertained by
measurement. This gives the pull of the two large balls upon the two
small ones. We next calculate what this pull would be were the balls as
far apart as the small balls are from the centre of the earth. We can
then form the following proportion: the pull of the large balls upon the
small ones is to the pull of the earth upon the small ones as the mass
of the large balls is to the mass of the earth, or as the weight of the
large balls is to the weight of the earth. Of course, the pull of the
earth upon the small balls is the weight of the small balls. In this way
it has been ascertained that the mass of the earth is about 5.6 times
that of a globe of water of the same size. In other words, the _mean
density_ of the earth is about 5.6.

[Illustration: Fig. 98.]

[Illustration: Fig. 99.]

The weight of the earth in pounds may be found by multiplying the number
of cubic feet in it by 62-1/2 (the weight, in pounds, of one cubic foot
of water), and this product by 5.6.

[Illustration: Fig. 100.]

86. _Cause of Precession._--We have seen that the earth is flattened at
the poles: in other words, the earth has the form of a sphere, with a
protuberant ring around its equator. This equatorial ring is inclined to
the plane of the ecliptic at an angle of about 23-1/2°. In Fig. 100 this
ring is represented as detached from the enclosed sphere. _S_ represents
the sun, and _Sc_ the ecliptic. As the point _A_ of the ring is nearer
the sun than the point _B_ is, the sun's pull upon _A_ is greater than
upon _B_: hence the sun tends to pull the ring over into the plane of
the ecliptic; but the rotation of the earth tends to keep the ring in
the same plane. The struggle between these two tendencies causes the
earth, to which the ring is attached, to wabble like a spinning-top,
whose rotation tends to keep it erect, while gravity tends to pull it
over. The handle of the top has a gyratory motion, which causes it to
describe a curve. The axis of the heavens corresponds to the handle of
the top.


                             II. THE MOON.


                      Distance, Size, and Motions.


87. _The Distance of the Moon._--The moon is the nearest of the heavenly
bodies. Its distance from the centre of the earth is only about sixty
times the radius of the earth, or, in round numbers, two hundred and
forty thousand miles.

    The ordinary method of finding the distance of one of the nearer
    heavenly bodies is first to ascertain its horizontal parallax. This
    enables us to form a right-angled triangle, the lengths of whose
    sides are easily computed, and the length of whose hypothenuse is
    the distance of the body from the centre of the earth.

[Illustration: Fig. 101.]

    Horizontal parallax has already been defined (32) as the
    displacement of a heavenly body when on the horizon, caused by its
    being seen from the surface, instead of the centre, of the earth.
    This displacement is due to the fact that the body is seen in a
    different direction from the surface of the earth from that in which
    it would be seen from the centre. Horizontal parallax might be
    defined as the difference in the directions in which a body on the
    horizon would be seen from the surface and from the centre of the
    earth. Thus, in Fig. 101, _C_ is the centre of the earth, _A_ a
    point on the surface, and _B_ a body on the horizon of _A_. _AB_ is
    the direction in which the body would be seen from _A_, and _CB_ the
    direction in which it would be seen from _C_. The difference of
    these directions, or the angle _ABC_, is the parallax of the body.

    The triangle _BAC_ is right-angled at _A_; the side _AC_ is the
    radius of the earth, and the hypothenuse is the distance of the body
    from the centre of the earth. When the parallax _ABC_ is known, the
    length of _CB_ can easily by found by trigonometrical computation.

    We have seen (32) that the parallax of a heavenly body grows less
    and less as the body passes from the horizon towards the zenith. The
    parallax of a body and its altitude are, however, so related, that,
    when we know the parallax at any altitude, we can readily compute
    the horizontal parallax.

    The usual method of finding the parallax of one of the nearer
    heavenly bodies is first to find its parallax when on the meridian,
    as seen from two places on the earth which differ considerably in
    latitude: then to calculate what would be the parallax of the body
    as seen from one of these places and the centre of the earth: and
    then finally to calculate what would be the parallax were the body
    on the horizon.

[Illustration: Fig. 102.]

    Thus, we should ascertain the parallax of the body _B_ (Fig. 102) as
    seen from _A_ and _D_, or the angle _ABD_. We should then calculate
    its parallax as seen from _A_ and _C_, or the angle _ABC_. Finally
    we should calculate what its parallax would be were the body on the
    horizon, or the angle _AB'C_.

    The simplest method of finding the parallax of a body _B_ (Fig. 102)
    as seen from the two points _A_ and _D_ is to compare its direction
    at each point with that of the same fixed star near the body. The
    star is so distant, that it will be seen in the same direction from
    both points: hence, if the direction of the body differs from that
    of the star 2° as seen from one point, and 2° 6' as seen from the
    other point, the two lines _AB_ and _DB_ must differ in direction by
    6'; in other words, the angle _ABD_ would be 6'.

    The method just described is the usual method of finding the
    parallax of the moon.

88. _The Apparent Size of the Moon._--The _apparent size_ of a body is
the visual angle subtended by it; that is, the angle formed by two lines
drawn from the eye to two opposite points on the outline of the body.
The apparent size of a body depends upon both its _magnitude_ and its
_distance_.

The apparent size, or _angular diameter_, of the moon is about
thirty-one minutes. This is ascertained by means of the wire micrometer
already described (19). The instrument is adjusted so that its
longitudinal wire shall pass through the centre of the moon, and its
transverse wires shall be tangent to the limbs of the moon on each side,
at the point where they are cut by the longitudinal wire. The micrometer
screw is then turned till the wires are brought together. The number of
turns of the screw needed to accomplish this will indicate the arc
between the wires, or the angular diameter of the moon.

[Illustration: Fig. 103.]

In order to be certain that the longitudinal wire shall pass through the
centre of the moon, it is best to take the moon when its disc is in the
form of a crescent, and to place the longitudinal wire against the
points, or _cusps_, of the crescent, as shown in Fig. 103.

[Illustration: Fig. 104.]

89. _The Real Size of the Moon._--The real diameter of the moon is a
little over one-fourth of that of the earth, or a little more than two
thousand miles. The comparative sizes of the earth and moon are shown in
Fig. 104.

[Illustration: Fig. 105.]

    The distance and apparent size of the moon being known, her real
    diameter is found by means of a triangle formed as shown in Fig.
    105. _C_ represents the centre of the moon, _CB_ the distance of the
    moon from the earth, and _CA_ the radius of the moon. _BAC_ is a
    triangle, right-angled at _A_. The angle _ABC_ is half the apparent
    diameter of the moon. With the angles _A_ and _B_, and the side _CB_
    known, it is easy to find the length of _AC_ by trigonometrical
    computation. Twice _AC_ will be the diameter of the moon.

The volume of the moon is about one-fiftieth of that of the earth.

90. _Apparent Size of the Moon on the Horizon and in the Zenith._.--The
moon is nearly four thousand miles farther from the observer when she is
on the horizon than when she is in the zenith. This is evident from Fig.
106. _C_ is the centre of the earth, _M_ the moon on the horizon, _M'_
the moon in the zenith, and _O_ the point of observation. _OM_ is the
distance of the moon when she is on the horizon, and _OM'_ the distance
of the moon from the observer when she is in the zenith. _CM_ is equal
to _CM'_, and _OM_ is about the length of _CM_; but _OM'_ is about four
thousand miles shorter than _CM'_: hence _OM'_ is about four thousand
miles shorter than _OM_.

[Illustration: Fig. 106.]

    Notwithstanding the moon is much nearer when at the zenith than at
    the horizon, it seems to us much larger at the horizon.

    This is a pure illusion, as we become convinced when we measure the
    disc with accurate instruments, so as to make the result independent
    of our ordinary way of judging. When the moon is near the horizon,
    it seems placed beyond all the objects on the surface of the earth
    in that direction, and therefore farther off than at the zenith,
    where no intervening objects enable us to judge of its distance. In
    any case, an object which keeps the same apparent magnitude seems to
    us, through the instinctive habits of the eye, the larger in
    proportion as we judge it to be more distant.

    91. _The Apparent Size of the Moon increased by Irradiation._--In
    the case of the moon, the word _apparent_ means much more than it
    does in the case of other celestial bodies. Indeed, its brightness
    causes our eyes to play us false. As is well known, the crescent of
    the new moon seems part of a much larger sphere than that which it
    has been said, time out of mind, to "hold in its arms." The bright
    portion of the moon as seen with our measuring instruments, as well
    as when seen with the naked eye, covers a larger space in the field
    of the telescope than it would if it were not so bright. This effect
    of _irradiation_, as it is called, must be allowed for in exact
    measurements of the diameter of the moon.

[Illustration: Fig. 107.]

92. _Apparent Size of the Moon in Different Parts of her Orbit._--Owing
to the eccentricity of the moon's orbit, her distance from the earth
varies somewhat from time to time. This variation causes a corresponding
variation in her apparent size, which is illustrated in Fig. 107.

93. _The Mass of the Moon._--The moon is considerably less dense than
the earth, its mass being only about one-eightieth of that of the earth;
that is, while it would take only about fifty moons to make the bulk of
the earth, it would take about eighty to make the mass of the earth.

    One method of finding the mass of the moon is to compare her effect
    in producing the _tides_ with that of the sun. We first calculate
    what would be the moon's effect in producing the tides, were she as
    far off as the sun. We then form the following proportion: as the
    sun's effect in producing the tides is to the moon's effect at the
    same distance, so is the mass of the sun to the mass of the moon.

    The method of finding the mass of the sun will be given farther on.

94. _The Orbital Motion of the Moon._--If we watch the moon from night
to night, we see that she moves eastward quite rapidly among the stars.
When the new moon is first visible, it appears near the horizon in the
west, just after sunset. A week later the moon will be on the meridian
at the same hour, and about a week later still on the eastern horizon.
The moon completes the circuit of the heavens in a period of about
thirty days, moving eastward at the rate of about twelve degrees a day.
This eastward motion of the moon is due to the fact that she is
revolving around the earth from west to east.

[Illustration: Fig. 108.]

95. _The Aspects of the Moon._--As the moon revolves around the earth,
she comes into different positions with reference to the earth and sun.
These different positions of the moon are called the _aspects_ of the
moon. The four chief aspects of the moon are shown in Fig. 108. When the
moon is at _M_, she appears in the opposite part of the heavens to the
sun, and is said to be in _opposition_; when at _M'_ and at _M'''_, she
appears ninety degrees away from the sun, and is said to be in
_quadrature_; when at _M''_, she appears in the same part of the heavens
as the sun, and is said to be in _conjunction_.

96. _The Sidereal and Synodical Periods of the Moon._--The _sidereal
period_ of the moon is the time it takes her to pass around from a star
to that star again, or the time it takes her to _make a complete
revolution around the earth_. This is a period of about twenty-seven
days and a third. It is sometimes called the _sidereal month_.

The _synodical period_ of the moon is the time that it takes the moon to
_pass from one aspect around to the same aspect again_. This is a period
of about twenty-nine days and a half, and it is sometimes called the
_synodical month_.

[Illustration: Fig. 109.]

The reason why the synodical period is longer than the sidereal period
will appear from Fig. 109. _S_ represents the position of the sun, _E_
that of the earth, and the small circle the orbit of the moon around the
earth. The arrow in the small circle represents the direction the moon
is revolving around the earth, and the arrow in the arc between _E_ and
_E'_ indicates the direction of the earth's motion in its orbit. When
the moon is at _M_{1}_, she is in conjunction. As the moon revolves
around the earth, the earth moves forward in its orbit. When the moon
has come round to _m_{1}_, so that _m_{3}m_{1}_ is parallel with
_M_{3}M_{1}_, she will have made a complete or _sidereal_ revolution
around the earth; but she will not be in conjunction again till she has
come round to _M_, so as again to be between the earth and sun. That is
to say, the moon must make more than a complete revolution in a
synodical period.

[Illustration: Fig. 110.]

    The greater length of the synodical period is also evident from Fig.
    110. _T_ represents the earth, and _L_ the moon. The arrows indicate
    the direction in which each is moving. When the earth is at _T_, and
    the moon at _L_, the latter is in conjunction. When the earth has
    reached _T'_, and the moon _L'_, the latter has made a sidereal
    revolution; but she will not be in conjunction again till the earth
    has reached _T''_, and the moon _L''_.

97. _The Phases of the Moon._--When the new moon appears in the west, it
has the form of a _crescent_, with its convex side towards the sun, and
its horns towards the east. As the moon advances towards quadrature, the
crescent grows thicker and thicker, till it becomes a _half-circle_ at
first quarter. When it passes quadrature, it begins to become convex
also on the side away from the sun, or _gibbous_ in form. As it
approaches opposition, it becomes more and more nearly circular, until
at opposition it is a _full_ circle. From full moon to last quarter it
is again gibbous, and at last quarter a half-circle. From last quarter
to new moon it is again crescent; but the horns of the crescent are now
turned towards the west. The successive phases of the moon are shown in
Fig. 111.

[Illustration: Fig. 111.]

98. _Cause of the Phases of the Moon._--Take a globe, half of which is
colored white and the other half black in such a way that the line which
separates the white and black portions shall be a great circle which
passes through the poles of the globe, and rotate the globe slowly, so
as to bring the white half gradually into view. When the white part
first comes into view, the line of separation between it and the black
part, which we may call the _terminator_, appears concave, and its
projection on a plane perpendicular to the line of vision is a concave
line. As more and more of the white portion comes into view, the
projection of the terminator becomes less and less concave. When half of
the white portion comes into view, the terminator is projected as a
straight line. When more than half of the white portion comes into view,
the terminator begins to appear as a convex line, and this line becomes
more and more convex till the whole of the white half comes into view,
when the terminator becomes circular.

[Illustration: Fig. 112.]

The moon is of itself a dark, opaque globe; but the half that is towards
the sun is always bright, as shown in Fig. 112. This bright half of the
moon corresponds to the white half of the globe in the preceding
illustration. As the moon revolves around the earth, different portions
of this illumined half are turned towards the earth. At new moon, when
the moon is in conjunction, the bright half is turned entirely away from
the earth, and the disc of the moon is black and invisible. Between new
moon and first quarter, less than half of the illumined side is turned
towards the earth, and we see this illumined portion projected as a
crescent. At first quarter, just half of the illumined side is turned
towards the earth, and we see this half projected as a half-circle.
Between first quarter and full, more than half of the illumined side is
turned towards the earth, and we see it as gibbous. At full, the whole
of the illumined side is turned towards us, and we see it as a full
circle. From full to new moon again, the phases occur in the reverse
order.

99. _The Form of the Moon's Orbit._--The orbit of the moon around the
earth is an ellipse of slight eccentricity. The form of this ellipse is
shown in Fig. 113. _C_ is the centre of the ellipse, and _E_ the
position of the earth at one of its foci. The eccentricity of the
ellipse is only about one-eighteenth. It is impossible for the eye to
distinguish such an ellipse from a circle.

[Illustration: Fig. 113.]

100. _The Inclination of the Moon's Orbit._--The plane of the moon's
orbit is inclined to the ecliptic by an angle of about five degrees. The
two points where the moon's orbit cuts the ecliptic are called her
_nodes_. The moon's nodes have a westward motion corresponding to that
of the equinoxes, but much more rapid. They complete the circuit of the
ecliptic in about nineteen years.

The moon's latitude ranges from 5° north to 5° south; and since, owing
to the motion of her nodes, the moon is, during a period of nineteen
years, 5° north and 5° south of every part of the ecliptic, her
declination will range from 23-1/2° + 5° = 28-1/2° north to 23-1/2° + 5°
= 28-1/2° south.

101. _The Meridian Altitude of the Moon._--The _meridian altitude_ of
any body is its altitude when on the meridian. In our latitude, the
meridian altitude of any point on the equinoctial is forty-nine degrees.
The meridian altitude of the summer solstice is 49° + 23-1/2° = 72-1/2°,
and that of the winter solstice is 49° - 23-1/2° = 25-1/2°. The greatest
meridian altitude of the moon is 72-1/2° + 5° = 77-1/2°, and its least
meridian altitude, 25-1/2° - 5° = 20-1/2°.

When the moon's meridian altitude is greater than the elevation of the
equinoctial, it is said to run _high_, and when less, to run _low_. The
full moon runs high when the sun is south of the equinoctial, and low
when the sun is north of the equinoctial. This is because the full moon
is always in the opposite part of the heavens to the sun.

    102. _Wet and Dry Moon._--At the time of new moon, the cusps of the
    crescent sometimes lie in a line which is nearly perpendicular with
    the horizon, and sometimes in a line which is nearly parallel with
    the horizon. In the former case the moon is popularly described as a
    _wet_ moon, and in the latter case as a _dry_ moon.

[Illustration: Fig. 114.]

    The great circle which passes through the centre of the sun and moon
    will pass through the centre of the crescent, and be perpendicular
    to the line joining the cusps. Now the ecliptic makes the least
    angle with the horizon when the vernal equinox is on the eastern
    horizon and the autumnal equinox is on the western. In our latitude,
    as we have seen, this angle is 25-1/2°: hence in our latitude, if
    the moon were at new on the ecliptic when the sun is at the autumnal
    equinox, as shown at _M_{3}_ (Fig. 114), the great circle passing
    through the centre of the sun and moon would be the ecliptic, and at
    New York would be inclined to the horizon at an angle of 25-1/2°. If
    the moon happened to be 5° south of the ecliptic at this time, as at
    _M_{4}_, the great circle passing through the centre of the sun and
    moon would make an angle of only 20-1/2° with the horizon. In either
    of these cases the line joining the cusps would be nearly
    perpendicular to the horizon.

[Illustration: Fig. 115.]

    If the moon were at new on the ecliptic when the sun is near the
    vernal equinox, as shown at _M_{1}_ (Fig. 115), the great circle
    passing through the centres of the sun and moon would make an angle
    of 72-1/2° with the horizon at New York; and were the moon 5° north
    of the ecliptic at that time, as shown at _M_{2}_, this great circle
    would make an angle of 77-1/2° with the horizon. In either of these
    cases, the line joining the cusps would be nearly parallel with the
    horizon.

    At different times, the line joining the cusps may have every
    possible inclination to the horizon between the extreme cases shown
    in Figs. 114 and 115.

103. _Daily Retardation of the Moon's Rising._--The moon rises, on the
average, about fifty minutes later each day. This is owing to her
eastward motion. As the moon makes a complete revolution around the
earth in about twenty-seven days, she moves eastward at the rate of
about thirteen degrees a day, or about twelve degrees a day faster than
the sun. Were the moon, therefore, on the horizon at any hour to-day,
she would be some twelve degrees below the horizon at the same hour
to-morrow. Now, as the horizon moves at the rate of one degree in four
minutes, it would take it some fifty minutes to come up to the moon so
as to bring her upon the horizon. Hence the daily retardation of the
moon's rising is about fifty minutes; but it varies considerably in
different parts of her orbit.

    There are two reasons for this variation in the daily retardation:--

    (1) The moon moves at a _varying rate in her orbit_; her speed being
    greatest at perigee, and least at apogee: hence, other things being
    equal, the retardation is greatest when the moon is at perigee, and
    least when she is at apogee.

[Illustration: Fig. 116.]

[Illustration: Fig. 117.]

    (2) The moon moves at a _varying angle to the horizon_. The moon
    moves nearly in the plane of the ecliptic, and of course she passes
    both equinoxes every lunation. When she is near the autumnal
    equinox, her path makes the greatest angle with the eastern horizon,
    and when she is near the vernal equinox, the least angle: hence the
    moon moves away from the horizon fastest when she is near the
    autumnal equinox, and slowest when she is near the vernal equinox.
    This will be evident from Figs. 116 and 117. In each figure, _SN_
    represents a portion of the eastern horizon, and _Ec_, _E'c'_, a
    portion of the ecliptic. _AE_, in Fig. 116, represents the autumnal
    equinox, and _AEM_ the daily motion of the moon. _VE_, in Fig. 117,
    represents the vernal equinox, and _VEM'_ the motion of the moon for
    one day. In the first case this motion would carry the moon away
    from the horizon the distance _AM_, and in the second case the
    distance _A'M'_. Now, it is evident that _AM_ is greater than
    _A'M'_: hence, other things being equal, the greatest retardation of
    the moon's rising will be when the moon is near the autumnal
    equinox, and the least retardation when the moon is near the vernal
    equinox.

The least retardation at New York is twenty-three minutes, and the
greatest an hour and seventeen minutes. The greatest and least
retardations vary somewhat from month to month; since they depend not
only upon the position of the moon in her orbit with reference to the
equinoxes, but also upon the latitude of the moon, and upon her nearness
to the earth.

[Illustration: Fig. 118.]

The direction of the moon's motion with reference to the ecliptic is
shown in Fig. 118, which shows the moon's motion for one day in July,
1876.

104. _The Harvest Moon_--The long and short retardations in the rising
of the moon, though they occur every month, are not likely to attract
attention unless they occur at the time of full moon. The long
retardations for full moon occur when the moon is near the autumnal
equinox at full. As the full moon is always opposite to the sun, the sun
must in this case be near the vernal equinox: hence the long
retardations for full moon occur in the spring, the greatest retardation
being in March.

The least retardations for full moon occur when the moon is near the
vernal equinox at full: the sun must then be near the autumnal equinox.
Hence the least retardations for full moon occur in the months of
August, September, and October. The retardation is, of course, least for
September; and the full moon of this month rises night after night less
than half an hour later than the previous night. The full moon of
September is called the "Harvest Moon," and that of October the
"Hunter's Moon."

105. _The Rotation of the Moon._--A careful examination of the spots on
the disc of the moon reveals the fact that she always presents the same
side to the earth. In order to do this, she must rotate on her axis
while making a revolution around the earth, or in about twenty-seven
days.

106. _Librations of the Moon._--The moon appears to rock slowly to and
fro, so as to allow us to see alternately a little farther around to the
right and the left, or above and below, than we otherwise could. This
apparent rocking of the moon is called _libration_. The moon has three
librations:--

(1) _Libration in Latitude._--This libration enables us to see
alternately a little way around on the northern and southern limbs of
the moon.

    This libration is due to the fact that the axis of the moon is not
    quite perpendicular to the plane of her orbit. The deviation from
    the perpendicular is six degrees and a half. As the axis of the
    moon, like that of the earth, maintains the same direction, the
    poles of the moon will be turned alternately six degrees and a half
    toward and from the earth.

(2) _Libration in Longitude._--This libration enables us to see
alternately a little farther around on the eastern and western limbs of
the moon.

[Illustration: Fig. 119.]

    It is due to the fact that the moon's axial motion is uniform, while
    her orbital motion is not. At perigee her orbital motion will be in
    advance of her axial motion, while at apogee the axial motion will
    be in advance of the orbital. In Fig. 119, _E_ represents the earth,
    _M_ the moon, the large arrow the direction of the moon's motion in
    her orbit, and the small arrow the direction of her motion of
    rotation. When the moon is at _M_, the line _AB_, drawn
    perpendicular to _EM_, represents the circle which divides the
    visible from the invisible portion of the moon. While the moon is
    passing from _M_ to _M'_, the moon performs less than a quarter of a
    rotation, so that _AB_ is no longer perpendicular to _EM'_. An
    observer on the earth can now see somewhat beyond _A_ on the western
    limb of the moon, and not quite up to _B_ on the eastern limb. While
    the moon is passing from _M'_ to _M''_, her axial motion again
    overtakes her orbital motion, so that the line _AB_ again becomes
    perpendicular to the line joining the centre of the moon to the
    centre of the earth. Exactly the same side is now turned towards the
    earth as when the moon was at _M_. While the moon passes from _M''_
    to _M'''_, her axial motion gets in advance of her orbital motion,
    so that _AB_ is again inclined to the line joining the centres of
    the earth and moon. A portion of the eastern limb of the moon beyond
    _B_ is now brought into view to the earth, and a portion of the
    western limb at _A_ is carried out of view. While the moon is
    passing from _M'''_ to _M_, the orbital motion again overtakes the
    axial motion, and _AB_ is again perpendicular to _ME_.

(3) _Parallactic Libration._--While an observer at the centre of the
earth would get the same view of the moon, whether she were on the
eastern horizon, in the zenith, or on the western horizon, an observer
on the surface of the earth does not get exactly the same view in these
three cases. When the moon is on the eastern horizon, an observer on the
surface of the earth would see a little farther around on the western
limb of the moon than when she is in the zenith, and not quite so far
around on the eastern limb. On the contrary, when the moon is on the
western horizon, an observer on the surface of the earth sees a little
farther around on the eastern limb of the moon than when she is in the
zenith, and not quite so far around on her western limb.

[Illustration: Fig. 120.]

    This will be evident from Fig. 120. _E_ is the centre of the earth,
    and _O_ a point on its surface. _AB_ is a line drawn through the
    centre of the moon, perpendicular to a line joining the centres of
    the moon and the earth. This line marks off the part of the moon
    turned towards the centre of the earth, and remains essentially the
    same during the day. _CD_ is a line drawn through the centre of the
    moon perpendicular to a line joining the centre of the moon and the
    point of observation. This line marks off the part of the moon
    turned towards _O_. When the moon is in the zenith, _CD_ coincides
    with _AB_; but, when the moon is on the horizon, _CD_ is inclined to
    _AB_. When the moon is on the eastern horizon, an observer at _O_
    sees a little beyond _B_, and not quite to _A_; and, when she is on
    the western horizon, he sees a little beyond _A_, and not quite to
    _B_. _B_ is on the western limb of the moon, and _A_ on her eastern
    limb.

    Since this libration is due to the point from which the moon is
    viewed, it is called _parallactic_ libration; and, since it occurs
    daily, it is called _diurnal_ libration.

[Illustration: Fig. 121.]

    107. _Portion of the Lunar Surface brought into View by
    Libration._--The area brought into view by the first two librations
    is between one-twelfth and one-thirteenth of the whole lunar
    surface, or nearly one-sixth of the hemisphere of the moon which is
    turned away from the earth when the moon is at her state of mean
    libration. Of course a precisely equal portion of the hemisphere
    turned towards us during mean libration is carried out of view by
    the lunar librations.

    If we add to each of these areas a fringe about one degree wide, due
    to the diurnal libration, and which we may call the _parallactic_
    fringe, we shall find that the total area brought into view is
    almost exactly one-eleventh part of the whole surface of the moon. A
    similar area is carried out of view; so that the whole region thus
    swayed out of and into view amounts to two-elevenths of the moon's
    surface. This area is shown in Fig. 121, which is a side view of the
    moon.

[Illustration: Fig. 122.]

    108. _The Moon's Path through Space._--Were the earth stationary,
    the moon would describe an ellipse around it similar to that of Fig.
    113; but, as the earth moves forward in her orbit at the same time
    that the moon revolves around it, the moon is made to describe a
    sinuous path, as shown by the continuous line in Fig. 122. This
    feature of the moon's path is greatly exaggerated in the upper
    portion of the diagram. The form of her path is given with a greater
    degree of accuracy in the lower part of the figure (the broken line
    represents the path of the earth); but even here there is
    considerable exaggeration. The complete serpentine path of the moon
    around the sun is shown, greatly exaggerated, in Fig. 123, the
    broken line being the path of the earth.

[Illustration: Fig. 123.]

    The path described by the moon through space is much the same as
    that described by a point on the circumference of a wheel which is
    rolled over another wheel. If we place a circular disk against the
    wall, and carefully roll along its edge another circular disk (to
    which a piece of lead pencil has been fastened so as to mark upon
    the wall), the curve described will somewhat resemble that described
    by the moon. This curve is called an _epicycloid_, and it will be
    seen that at every point it is concave towards the centre of the
    larger disk. In the same way the moon's orbit is _at every point
    concave towards the sun_.

[Illustration: Fig. 124.]

    The exaggeration of the sinuosity in Fig. 123 will be more evident
    when it is stated, that, on the scale of Fig. 124, the whole of the
    serpentine curve would lie _within the breadth_ of the fine circular
    line _MM'_.

109. _The Lunar Day._--The lunar day is twenty-nine times and a half as
long as the terrestrial day. Near the moon's equator the sun shines
without intermission nearly fifteen of our days, and is absent for the
same length of time. Consequently, the vicissitudes of temperature to
which the surface is exposed must be very great. During the long lunar
night the temperature of a body on the moon's surface would probably
fall lower than is ever known on the earth, while during the day it must
rise higher than anywhere on our planet.

[Illustration: Fig. 125.]

    It might seem, that, since the moon rotates on her axis in about
    twenty-seven days, the lunar day ought to be twenty-seven days long,
    instead of twenty-nine. There is, however, a solar, as well as a
    sidereal, day at the moon, as on the earth; and the solar day at the
    moon is longer than the sidereal day, for the same reason as on the
    earth. During the solar day the moon must make both a _synodical
    rotation_ and a _synodical revolution_. This will be evident from
    Fig. 125, in which is shown the path of the moon during one complete
    lunation. _E_, _E'_, _E''_, etc., are the successive positions of
    the earth; and 1, 2, 3, 4, 5, the successive positions of the moon.
    The small arrows indicate the direction of the moon's rotation. The
    moon is full at 1 and 5. At 1, _A_, at the centre of the moon's
    disk, will have the sun, which lies in the direction _AS_, upon the
    meridian. Before _A_ will again have the sun on the meridian, the
    moon must have made a synodical revolution; and, as will be seen by
    the dotted lines, she must have made more than a complete rotation.
    The rotation which brings the point _A_ into the same relation to
    the earth and sun is called a _synodical_ rotation.

    It will also be evident from this diagram that the moon must make a
    synodical rotation during a synodical revolution, in order always to
    present the same side to the earth.

110. _The Earth as seen from the Moon._--To an observer on the moon, the
earth would be an immense moon, going through the same phases that the
moon does to us; but, instead of rising and setting, it would only
oscillate to and fro through a few degrees. On the other side of the
moon it would never be seen at all. The peculiarities of the moon's
motions which cause the librations, and make a spot on the moon's disk
seem to an observer on the earth to oscillate to and fro, would cause
the earth as a whole to appear to a lunar observer to oscillate to and
fro in the heavens in a similar manner.

It is a well-known fact, that, at the time of new moon, the dark part of
the moon's surface is partially illumined, so that it becomes visible to
the naked eye. This must be due to the light reflected to the moon from
the earth. Since at new moon the moon is between the earth and sun, it
follows, that, when it is new moon at the earth, it must be _full earth_
at the moon: hence, while the bright crescent is enjoying full sunlight,
the dark part of its surface is enjoying the light of the full _earth_.
Fig. 126 represents the full earth as seen from the moon.

[Illustration: Fig. 126.]


                      The Atmosphere of the Moon.


111. _The Moon has no Appreciable Atmosphere._--There are several
reasons for believing that the moon has little or no atmosphere.

(1) Had the moon an atmosphere, it would be indicated at the time of a
solar eclipse, when the moon passes over the disk of the sun. If the
atmosphere were of any considerable density, it would absorb a part of
the sun's rays, so as to produce a dusky border in front of the moon's
disk, as shown in Fig. 127. In reality no such dusky border is ever
seen; but the limb of the moon appears sharp, and clearly defined, as in
Fig. 128.

[Illustration: Fig. 127.]

[Illustration: Fig. 128.]

If the atmosphere were not dense enough to produce this dusky border,
its refraction would be sufficient to distort the delicate cusps of the
sun's crescent in the manner shown at the top of Fig. 125; but no such
distortion is ever observed. The cusps always appear clear and sharp, as
shown at the bottom of the figure: hence it would seem that there can be
no atmosphere of appreciable density at the moon.

(2) The absence of an atmosphere from the moon is also shown by the
absence of twilight and of diffused daylight.

Upon the earth, twilight continues until the sun is eighteen degrees
below the horizon; that is, day and night are separated by a belt twelve
hundred miles in breadth, in which the transition from light to darkness
is gradual. We have seen (66) that this twilight results from the
refraction and reflection of light by our atmosphere; and, if the moon
had an atmosphere, we should notice a similar gradual transition from
the bright to the dark portions of her surface. Such, however, is not
the case. The boundary between the light and darkness, though irregular,
is sharply defined. Close to this boundary the unillumined portion of
the moon appears just as dark as at any distance from it.

The shadows on the moon are also pitchy black, without a trace of
diffused daylight.

[Illustration: Fig. 129.]

    (3) The absence of an atmosphere is also proved by the absence of
    refraction when the moon passes between us and the stars. Let _AB_
    (Fig. 129) represent the disk of the moon, and _CD_ an atmosphere
    supposed to surround it. Let _SAE_ represent a straight line from
    the earth, touching the moon at _A_, and let _S_ be a star situated
    in the direction of this line. If the moon had no atmosphere, this
    star would appear to touch the edge of the moon at _A_; but, if the
    moon had an atmosphere, a star behind the edge of the moon, at _S'_,
    would be visible at the earth; for the ray _S'A_ would be bent by
    the atmosphere into the direction _AE'_. So, also, on the opposite
    side of the moon, a star might be seen at the earth, although really
    behind the edge of the moon: hence, if the moon had an atmosphere,
    the time during which a star would be concealed by the moon would be
    less than if it had no atmosphere, and the amount of this effect
    must be proportional to the density of the atmosphere.

    The moon, in her orbital course across the heavens, is continually
    passing before, or _occulting_, some of the stars that so thickly
    stud her apparent path; and when we see a star thus pass behind the
    lunar disk on one side, and come out again on the other side, we are
    virtually observing the setting and rising of that star upon the
    moon. The moon's apparent diameter has been measured over and over
    again, and is known with great accuracy; the rate of her motion
    across the sky is also known with perfect accuracy: hence it is easy
    to calculate how long the moon will take to travel across a part of
    the sky exactly equal in length to her own diameter. Supposing,
    then, that we observe a star pass behind the moon, and out again, it
    is clear, that, if there is no atmosphere, the interval of time
    during which it remains occulted ought to be exactly equal to the
    computed time which the moon would take to pass over the star. If,
    however, from the existence of a lunar atmosphere, the star
    disappears too late, and re-appears too soon, as we have seen it
    would, these two intervals will not agree; the computed time will be
    greater than the observed time, and the difference will represent
    the amount of refraction the star's light has sustained or suffered,
    and hence the extent of atmosphere it has had to pass through.

    Comparisons of these two intervals of time have been repeatedly
    made, the most extensive being executed under the direction of the
    Astronomer Royal of England, several years ago, and based upon no
    less than two hundred and ninety-six occultation observations. In
    this determination the measured or telescopic diameter of the moon
    was compared with the diameter deduced from the occultations; and it
    was found that the telescopic diameter was greater than the
    occultation diameter by two seconds of angular measurement, or by
    about a thousandth part of the whole diameter of the moon. This
    discrepancy is probably due, in part at least, to _irradiation_
    (91), which augments the apparent size of the moon, as seen in the
    telescope as well as with the naked eye; but, if the whole two
    seconds were caused by atmospheric refraction, this would imply a
    horizontal refraction of one second, which is only one
    two-thousandth of the earth's horizontal refraction. It is possible
    that an atmosphere competent to produce this refraction would not
    make itself visible in any other way.

    But an atmosphere two thousand times rarer than our air can scarcely
    be regarded as an atmosphere at all. The contents of an air-pump
    receiver can seldom be rarefied to a greater extent than to about a
    thousandth of the density of air at the earth's surface; and the
    lunar atmosphere, if it exists at all, is thus proved to be twice as
    attenuated as what we commonly call a vacuum.


                        The Surface of the Moon.


[Illustration: Fig. 130.]

112. _Dusky Patches on the Disk of the Moon._--With the naked eye, large
dusky patches are seen on the moon, in which popular fancy has detected
a resemblance to a human face. With a telescope of low power, these dark
patches appear as smooth as water, and they were once supposed to be
seas. This theory was the origin of the name _mare_ (Latin for _sea_),
which is still applied to the larger of these plains; but, if there were
water on the surface of the moon, it could not fail to manifest its
presence by its vapor, which would form an appreciable atmosphere.
Moreover, with a high telescopic power, these plains present a more or
less uneven surface; and, as the elevations and depressions are found to
be permanent, they cannot, of course, belong to the surface of water.

    The chief of these plains are shown in Fig. 130. They are _Mare
    Crisium_, _Mare Foecunditatis_, _Mare Nectaris_, _Mare
    Tranquillitatis_, _Mare Serenitatis_, _Mare Imbrium_, _Mare
    Frigoris_, and _Oceanus Procellarum_. All these plains can easily be
    recognized on the surface of the full moon with the unaided eye.

113. _The Terminator of the Moon._--The terminator of the moon is the
line which separates the bright and dark portions of its disk. When
viewed with a telescope of even moderate power, the terminator is seen
to be very irregular and uneven. Many bright points are seen just
outside of the terminator in the dark portion of the disk, while all
along in the neighborhood of the terminator are bright patches and dense
shadows. These appearances are shown in Figs. 131 and 132, which
represent the moon near the first and last quarters. They indicate that
the surface of the moon is very rough and uneven.

[Illustration: Fig. 131.]

[Illustration: Fig. 132.]

As it is always either sunrise or sunset along the terminator, the
bright spots outside of it are clearly the tops of mountains, which
catch the rays of the sun while their bases are in the shade. The bright
patches in the neighborhood of the terminator are the sides of hills and
mountains which are receiving the full light of the sun, while the dense
shadows near by are cast by these elevations.

114. _Height of the Lunar Mountains._--There are two methods of finding
the height of lunar mountains:--

(1) We may measure the length of the shadows, and then calculate the
height of the mountains that would cast such shadows with the sun at the
required height above the horizon.

    The length of a shadow may be obtained by the following method: the
    longitudinal wire of the micrometer (19) is adjusted so as to pass
    through the shadow whose length is to be measured, and the
    transverse wires are placed one at each end of the shadow, as shown
    in Fig. 133. The micrometer screw is then turned till the wires are
    brought together, so as to ascertain the length of the arc between
    them. We may then form the proportion: the number of seconds in the
    semi-diameter of the moon is to the number of seconds in the length
    of the shadow, as the length of the moon's radius in miles to the
    length of the shadow in miles.

[Illustration: Fig. 133.]

    The height of the sun above the horizon is ascertained by measuring
    the angular distance of the mountain from the terminator.

(2) We may measure the distance of a bright point from the terminator,
and then construct a right-angled triangle, as shown in Fig. 134. A
solution of this triangle will enable us to ascertain the height of the
mountain whose top is just catching the level rays of the sun.

[Illustration: Fig. 134.]

    _B_ is the centre of the moon, _M_ the top of the mountain, and
    _SAM_ a ray of sunlight which just grazes the terminator at _A_, and
    then strikes the top of the mountain at _M_. The triangle _BAM_ is
    right-angled at _A_. _BA_ is the radius of the moon, and _AM_ is
    known by measurement; _BM_, the hypothenuse, may then be found by
    computation. _BM_ is evidently equal to the radius of the moon
    _plus_ the height of the mountain.

By one or the other of these methods, the heights of the lunar mountains
have been found with a great degree of accuracy. It is claimed that the
heights of the lunar mountains are more accurately known than those of
the mountains on the earth. Compared with the size of the moon, lunar
mountains attain a greater height than those on the earth.

115. _General Aspect of the Lunar Surface._--A cursory examination of
the moon with a low power is sufficient to show the prevalence of
crater-like inequalities and the general tendency to _circular_ shape
which is apparent in nearly all the surface markings; for even the large
"seas" and the smaller patches of the same character repeat in their
outlines the round form of the craters. It is along the terminator that
we see these crater-like spots to the best advantage; as it is there
that the rising or setting sun casts long shadows over the lunar
landscape, and brings elevations into bold relief. They vary greatly in
size; some being so large as to bear a sensible proportion to the moon's
diameter, while the smallest are so minute as to need the most powerful
telescopes and the finest conditions of atmosphere to perceive them.

[Illustration: Fig. 135.]

The prevalence of ring-shaped mountains and plains willbe evident from
Fig. 135, which is from a photograph of a model of the moon constructed
by Nasmyth.

This same feature is nearly as marked in Figs. 131 and 132, which are
copies of Rutherfurd's photographs of the moon.

116. _Lunar Craters._--The smaller saucer-shaped formations on the
surface of the moon are called _craters_. They are of all sizes, from a
mile to a hundred and fifty miles in diameter; and they are supposed to
be of volcanic origin. A high telescopic power shows that these craters
vary remarkably, not only in size, but also in structure and
arrangement. Some are considerably elevated above the surrounding
surface, others are basins hollowed out of that surface, and with low
surrounding ramparts; some are like walled plains, while the majority
have their lowest depression considerably below the surrounding surface;
some are isolated upon the plains, others are thickly crowded together,
overlapping and intruding upon each other; some have elevated peaks or
cones in their centres, and some are without these central cones, while
others, again, contain several minute craters instead; some have their
ramparts whole and perfect, others have them broken or deformed, and
many have them divided into terraces, especially on their inner sides.

A typical lunar crater is shown in Fig. 136.

[Illustration: Fig. 136.]

It is not generally believed that any active volcanoes exist on the moon
at the present time, though some observers have thought they discerned
indications of such volcanoes.

[Illustration: Fig. 137.]

117. _Copernicus._--This is one of the grandest of lunar craters (Fig.
137). Although its diameter (forty-six miles) is exceeded by others,
yet, taken as a whole, it forms one of the most impressive and
interesting objects of its class. Its situation, near the centre of the
lunar disk, renders all its wonderful details conspicuous, as well as
those of objects immediately surrounding it. Its vast rampart rises to
upwards of twelve thousand feet above the level of the plateau, nearly
in the centre of which stands a magnificent group of cones, three of
which attain a height of more than twenty-four hundred feet.

Many ridges, or spurs, may be observed leading away from the outer banks
of the great rampart. Around the crater, extending to a distance of more
than a hundred miles on every side, there is a complex network of bright
streaks, which diverge in all directions. These streaks do not appear in
the figure, nor are they seen upon the moon, except at and near the full
phase. They show conspicuously, however, by their united lustre on the
full moon.

This crater is seen just to the south-west of the large dusky plain in
the upper part of Fig. 132. This plain is _Mare Imbrium_, and the
mountain-chain seen a little to the right of Copernicus is named the
_Apennines_. Copernicus is also seen in Fig. 135, a little to the left
of the same range.

Under circumstances specially favorable, myriads of comparatively minute
but perfectly formed craters may be observed for more than seventy miles
on all sides around Copernicus. The district on the south-east side is
specially rich in these thickly scattered craters, which we have reason
to suppose stand over or upon the bright streaks.

118. _Dark Chasms._--Dark cracks, or chasms, have been observed on
various parts of the moon's surface. They sometimes occur singly, and
sometimes in groups. They are often seen to radiate from some central
cone, and they appear to be of volcanic origin. They have been called
_canals_ and _rills_.

[Illustration: Fig. 138.]

One of the most remarkable groups of these chasms is that to the west of
the crater named _Triesneker_. The crater and the chasms are shown in
Fig. 138. Several of these great cracks obviously diverge from a small
crater near the west bank of the great one, and they subdivide as they
extend from the apparent point of divergence, while they are crossed by
others. These cracks, or chasms, are nearly a mile broad at the widest
part, and, after extending full a hundred miles, taper away till they
become invisible.

[Illustration: Fig. 139.]

119. _Mountain-Ranges._--There are comparatively few mountain-ranges on
the moon. The three most conspicuous are those which partially enclose
Mare Imbrium; namely, the _Apennines_ on the south, and the _Caucasus_
and the _Alps_ on the east and north-east. The Apennines are the most
extended of these, having a length of about four hundred and fifty
miles. They rise gradually, from a comparatively level surface towards
the south-west, in the form of innumerable small elevations, which
increase in number and height towards the north-east, where they
culminate in a range of peaks whose altitude and rugged aspect must form
one of the most terribly grand and romantic scenes which imagination can
conceive. The north-east face of the range terminates abruptly in an
almost vertical precipice; while over the plain beneath, intensely black
spire-like shadows are cast, some of which at sunrise extend full ninety
miles, till they lose themselves in the general shading due to the
curvature of the lunar surface. Many of the peaks rise to heights of
from eighteen thousand to twenty thousand feet above the plain at their
north-east base (Fig. 139).

[Illustration: Fig. 140.]

Fig. 140 represents an ideal lunar landscape near the base of such a
lunar range. Owing to the absence of an atmosphere, the stars will be
visible in full daylight.

[Illustration: Fig. 141.]

120. _The Valley of the Alps._--The range of the _Alps_ is shown in Fig.
141. The great crater at the north end of this range is named _Plato_.
It is seventy miles in diameter.

The most remarkable feature of the Alps is the valley near the centre of
the range. It is more than seventy-five miles long, and about six miles
wide at the broadest part. When examined under favorable circumstances,
with a high magnifying power, it is seen to be a vast flat-bottomed
valley, bordered by gigantic mountains, some of which attain heights of
ten thousand feet or more.

[Illustration: Fig. 142.]

121. _Isolated Peaks._--There are comparatively few isolated peaks to be
found on the surface of the moon. One of the most remarkable of these is
that known as _Pico_, and shown in Fig. 142. Its height exceeds eight
thousand feet, and it is about three times as long at the base as it is
broad. The summit is cleft into three peaks, as is shown by the
three-peaked shadow it casts on the plain.

122. _Bright Rays._--About the time of full moon, with a telescope of
moderate power, a number of bright lines may be seen radiating from
several of the lunar craters, extending often to the distance of
hundreds of miles. These streaks do not arise from any perceptible
difference of level of the surface, they have no very definite outline,
and they do not present any sloping sides to catch more sunlight, and
thus shine brighter, than the general surface. Indeed, one great
peculiarity of them is, that they come out most forcibly when the sun is
shining perpendicularly upon them: hence they are best seen when the
moon is at full, and they are not visible at all at those regions upon
which the sun is rising or setting. They are not diverted by elevations
in their path, but traverse in their course craters, mountains, and
plains alike, giving a slight additional brightness to all objects over
which they pass, but producing no other effect upon them. "They look as
if, after the whole surface of the moon had assumed its final
configuration, a vast brush charged with a whitish pigment had been
drawn over the globe in straight lines, radiating from a central point,
leaving its trail upon every thing it touched, but obscuring nothing."

[Illustration: Fig. 143.]

The three most conspicuous craters from which these lines radiate are
_Tycho_, _Copernicus_, and _Kepler_. Tycho is seen at the bottom of
Figs. 143 and 130. Kepler is a little to the left of Copernicus in the
same figures.

It has been thought that these bright streaks are chasms which have been
filled with molten lava, which, on cooling, would afford a smooth
reflecting surface on the top.

123. _Tycho._--This crater is fifty-four miles in diameter, and about
sixteen thousand feet deep, from the highest ridge of the rampart to the
surface of the plateau, whence rises a central cone five thousand feet
high. It is one of the most conspicuous of all the lunar craters; not so
much on account of its dimensions as from its being the centre from
whence diverge those remarkable bright streaks, many of which may be
traced over a thousand miles of the moon's surface (Fig. 143). Tycho
appears to be an instance of a vast disruptive action which rent the
solid crust of the moon into radiating fissures, which were subsequently
filled with molten matter, whose superior luminosity marks the course of
the cracks in all directions from the crater as their common centre. So
numerous are these bright streaks when examined by the aid of the
telescope, and they give to this region of the moon's surface such
increased luminosity, that, when viewed as a whole, the locality can be
distinctly seen at full moon by the unassisted eye, as a bright patch of
light on the southern portion of the disk.


                  III. INFERIOR AND SUPERIOR PLANETS.


                           Inferior Planets.


124. _The Inferior Planets._--The _inferior planets_ are those which lie
between the earth and the sun, and whose orbits are included by that of
the earth. They are _Mercury_ and _Venus_.

[Illustration: Fig. 144.]

125. _Aspects of an Inferior Planet._--The four chief _aspects_ of an
inferior planet as seen from the earth are shown in Fig. 144, in which
_S_ represents the sun, _P_ the planet, and _E_ the earth.

When the planet is between the earth and the sun, as at _P_, it is said
to be in _inferior conjunction_.

When it is in the same direction as the sun, but beyond it, as at _P''_,
it is said to be in _superior conjunction_.

When the planet is at such a point in its orbit that a line drawn from
the earth to it would be tangent to the orbit, as at _P'_ and _P'''_, it
is said to be at its _greatest elongation_.

[Illustration: Fig. 145.]

126. _Apparent Motion of an Inferior Planet._--When the planet is at
_P_, if it could be seen at all, it would appear in the heavens at _A_.
As it moves from _P_ to _P'_, it will appear to move in the heavens from
_A_ to _B_. Then, as it moves from _P'_ to _P''_, it will appear to move
back again from _B_ to _A_. While it moves from _P''_ to _P'''_, it will
appear to move from _A_ to _C_; and, while moving from _P'''_ to _P_, it
will appear to move back again from _C_ to _A_. Thus the planet will
appear to oscillate to and fro across the sun from _B_ to _C_, never
getting farther from the sun than _B_ on the west, or _C_ on the east:
hence, when at these points, it is said to be at its _greatest western_
and _eastern elongations_. This oscillating motion of an inferior planet
across the sun, combined with the sun's motion among the stars, causes
the planet to describe a path among the stars similar to that shown in
Fig. 145.

[Illustration: Fig. 146.]

127. _Phases of an Inferior Planet._--An inferior planet, when viewed
with a telescope, is found to present a succession of phases similar to
those of the moon. The reason of this is evident from Fig. 146. As an
inferior planet passes around the sun, it presents sometimes more and
sometimes less of its bright hemisphere to the earth. When the earth is
at _T_, and Venus at superior conjunction, the planet turns the whole of
its bright hemisphere towards the earth, and appears _full_; it then
becomes _gibbous_, _half_, and _crescent_. When it comes into _inferior
conjunction_, it turns its dark hemisphere towards the earth: it then
becomes _crescent_, _half_, _gibbous_, and _full_ again.

128. _The Sidereal and Synodical Periods of an Inferior Planet._--The
time it takes a planet to make a complete revolution around the sun is
called the _sidereal period_ of the planet; and the time it takes it to
pass from one aspect around to the same aspect again, its _synodical
period_.

[Illustration: Fig. 147.]

The synodical period of an inferior planet is longer than its sidereal
period. This will be evident from an examination of Fig. 147. _S_ is the
position of the sun, _E_ that of the earth, and _P_ that of the planet
at inferior conjunction. Before the planet can be in inferior
conjunction again, it must pass entirely around its orbit, and overtake
the earth, which has in the mean time passed on in its orbit to _E'_.

While the earth is passing from _E_ to _E'_, the planet passes entirely
around its orbit, and from _P_ to _P'_ in addition. Now the arc _PP'_ is
just equal to the arc _EE'_: hence the planet has to pass over the same
arc that the earth does, and 360° more. In other words, the planet has
to gain 360° on the earth.

The synodical period of the planet is found by direct observation.

    129. _The Length of the Sidereal Period._--The length of the
    sidereal period of an inferior planet may be found by the following
    computation:--

        Let _a_ denote the synodical period of the planet,
        Let _b_ denote the sidereal period of the earth,
        Let _x_ denote the sidereal period of the planet.
        Then _360°/b_ = the daily motion of the earth,
        And _360°/x_ = the daily motion of the planet,
        And _360°/x - 360°/b_ = the daily gain of the planet:
        Also _360°/a_ = the daily gain of the planet:
        Hence _360°/x - 360°/b = 360°/a_.
        Dividing by 360°, we have _1/x - 1/b = 1/a_;
        Clearing of fractions, we have _ab - ax = bx_:
        Transposing and collecting, we have _(a + b)x = ab_:

        Therefore _x = ab/a+b_.

    130. _The Relative Distance of an Inferior Planet._--By the
    _relative distance_ of a planet, we mean its distance from the sun
    compared with the earth's distance from the sun. The relative
    distance of an inferior planet may be found by the following
    method:--

[Illustration: Fig. 148.]

    Let _V_, in Fig. 148, represent the position of Venus at its
    greatest elongation from the sun, _S_ the position of the sun, and
    _E_ that of the earth. The line _EV_ will evidently be tangent to a
    circle described about the sun with a radius equal to the distance
    of Venus from the sun at the time of this greatest elongation. Draw
    the radius _SV_ and the line _SE_. Since _SV_ is a radius, the angle
    at _V_ is a right angle. The angle at _E_ is known by measurement,
    and the angle at _S_ is equal to 90°- the angle _E_. In the
    right-angled triangle _EVS_, we then know the three angles, and we
    wish to find the ratio of the side _SV_ to the side _SE_.

    The ratio of these lines may be found by trigonometrical computation
    as follows:--

        _VS : ES = sin SEV : 1._

    Substitute the value of the sine of SEV, and we have

        _VS : ES = .723 : 1._

    Hence the relative distances of Venus and of the earth from the sun
    are .723 and 1.


                           Superior Planets.


131. _The Superior Planets._--The _superior planets_ are those which lie
beyond the earth. They are _Mars_, the _Asteroids_, _Jupiter_, _Saturn_,
_Uranus_, and _Neptune_.

[Illustration: Fig. 149.]

132. _Apparent Motion of a Superior Planet._--In order to deduce the
apparent motion of a superior planet from the real motions of the earth
and planet, let _S_ (Fig. 149) be the place of the sun; 1, 2, 3, etc.,
the orbit of the earth; _a_, _b_, _c_, etc., the orbit of Mars; and
_CGL_ a part of the starry firmament. Let the orbit of the earth be
divided into twelve equal parts, each described in one month; and let
_ab_, _bc_, _cd_, etc., be the spaces described by Mars in the same
time. Suppose the earth to be at the point 1 when Mars is at the point
_a_, Mars will then appear in the heavens in the direction of 1 _a_.
When the earth is at 3, and Mars at _c_, he will appear in the heavens
at _C_. When the earth arrives at 4, Mars will arrive at _d_, and will
appear in the heavens at _D_. While the earth moves from 4 to 5 and from
5 to 6, Mars will appear to have advanced among the stars from _D_ to
_E_ and from _E_ to _F_, in the direction from west to east. During the
motion of the earth from 6 to 7 and from 7 to 8, Mars will appear to go
backward from _F_ to _G_ and from _G_ to _H_, in the direction from east
to west. During the motion of the earth from 8 to 9 and from 9 to 10,
Mars will appear to advance from _H_ to _I_ and from _I_ to _K_, in the
direction from west to east, and the motion will continue in the same
direction until near the succeeding opposition.

The apparent motion of a superior planet projected on the heavens is
thus seen to be similar to that of an inferior planet, except that, in
the latter case, the retrogression takes place near inferior
conjunction, and in the former it takes place near opposition.

[Illustration: Fig. 150.]

133. _Aspects of a Superior Planet._--The four aspects of a superior
planet are shown in Fig. 150, in which _S_ is the position of the sun,
_E_ that of the earth, and _P_ that of the planet.

When the planet is on the opposite side of the earth to the sun, as at
_P_, it is said to be in _opposition_. The sun and the planet will then
appear in opposite parts of the heavens, the sun appearing at _C_, and
the planet at _A_.

When the planet is on the opposite side of the sun to the earth, as at
_P''_, it is said to be in _superior conjunction_. It will then appear
in the same part of the heavens as the sun, both appearing at _C_.

When the planet is at _P'_ and _P'''_, so that a line drawn from the
earth through the planet will make a right angle with a line drawn from
the earth to the sun, it is said to be in _quadrature_. At _P'_ it is in
its western quadrature, and at _P'''_ in its eastern quadrature.

[Illustration: Fig. 151.]

134. _Phases of a Superior Planet._--Mars is the only one of the
superior planets that has appreciable phases. At quadrature, as will
appear from Fig. 151, Mars does not present quite the same side to the
earth as to the sun: hence, near these parts of its orbit, the planet
appears slightly gibbous. Elsewhere in its orbit, the planet appears
full.

All the other superior planets are so far away from the sun and earth,
that the sides which they turn towards the sun and the earth in every
part of their orbit are so nearly the same, that no change in the form
of their disks can be detected.

135. _The Synodical Period of a Superior Planet._--During a synodical
period of a superior planet the earth must gain one revolution, or 360°,
on the planet, as will be evident from an examination of Fig. 152, in
which _S_ represents the sun, _E_ the earth, and _P_ the planet at
opposition. Before the planet can be in opposition again, the earth must
make a complete revolution, and overtake the planet, which has in the
mean time passed on from _P_ to _P'_.

[Illustration: Fig. 152.]

In the case of most of the superior planets the synodical period is
shorter than the sidereal period; but in the case of Mars it is longer,
since Mars makes more than a complete revolution before the earth
overtakes it.

The synodical period of a superior planet is found by direct
observation.

    136. _The Sidereal Period of a Superior Planet._--The sidereal
    period of a superior planet is found by a method of computation
    similar to that for finding the sidereal period of an inferior
    planet:--

        Let _a_ denote the synodical period of the planet,
        Let _b_ denote the sidereal period of the earth,
        Let _x_ denote the sidereal period of the planet.
        Then will _360°/b_ = daily motion of the earth,
        And _360°/x_ = daily motion of the planet;
        Also _360°/b - 360°/x_ = daily gain of the earth.
        But _360°/a_ = daily gain of the earth:
        Hence _360°/b - 360°/x = 360°/a_

        _1/b - 1/x = 1/a_

        _ax - ab = bx_

        _(a-b)x = ab_

        _x = ab/(a-b)_.

[Illustration: Fig. 153.]

    137. _The Relative Distance of a Superior Planet._--Let _S_, _e_,
    and _m_, in Fig. 153, represent the relative positions of the sun,
    the earth, and Mars, when the latter planet is in opposition. Let
    _E_ and _M_ represent the relative positions of the earth and Mars
    the day after opposition. At the first observation Mars will be seen
    in the direction _emA_, and at the second observation in the
    direction _EMA_.

    But the fixed stars are so distant, that if a line, _eA_, were drawn
    to a fixed star at the first observation, and a line, _EB_, drawn
    from the earth to the same fixed star at the second observation,
    these two lines would be sensibly parallel; that is, the fixed star
    would be seen in the direction of the line _eA_ at the first
    observation, and in the direction of the line _EB_, parallel to
    _eA_, at the second observation. But if Mars were seen in the
    direction of the fixed star at the first observation, it would
    appear back, or west, of that star at the second observation by the
    angular distance _BEA_; that is, the planet would have retrograded
    that angular distance. Now, this retrogression of Mars during one
    day, at the time of opposition, can be measured directly by
    observation. This measurement gives us the value of the angle _BEA_;
    but we know the rate at which both the earth and Mars are moving in
    their orbits, and from this we can easily find the angular distance
    passed over by each in one day. This gives us the angles _ESA_ and
    _MSA_. We can now find the relative length of the lines _MS_ and
    _ES_ (which represent the distances of Mars and of the earth from
    the sun), both by construction and by trigonometrical computation.

    Since _EB_ and _eA_ are parallel, the angle _EAS_ is equal to _BEA_.

        _SEA = 180° - (ESA + EAS)_
        _ESM = ESA - MSA_
        _EMS = 180° - (SEA + ESM)_.

    We have then

        _MS : ES = sin SEA : sin EMS._

    Substituting the values of the sines, and reducing the ratio to its
    lowest terms, we have

        _MS : ES = 1.524 : 1._

    Thus we find that the relative distances of Mars and the earth from
    the sun are 1.524 and 1. By the simple observation of its greatest
    elongation, we are able to determine the relative distances of an
    inferior planet and the earth from the sun; and, by the equally
    simple observation of the daily retrogression of a superior planet,
    we can find the relative distances of such a planet and the earth
    from the sun.


                              IV. THE SUN.


                 I. MAGNITUDE AND DISTANCE OF THE SUN.


[Illustration: Fig. 154.]

138. _The Volume of the Sun._--The apparent diameter of the sun is about
32', being a little greater than that of the moon. The real diameter of
the sun is 866,400 miles, or about a hundred and nine times that of the
earth.

As the diameter of the moon's orbit is only about 480,000 miles, or some
sixty times the diameter of the earth, it follows that the diameter of
the sun is nearly double that of the moon's orbit: hence, were the
centre of the sun placed at the centre of the earth, the sun would
completely fill the moon's orbit, and reach nearly as far beyond it in
every direction as it is from the earth to the moon. The circumference
of the sun as compared with the moon's orbit is shown in Fig. 154.

The volume of the sun is 1,305,000 times that of the earth.

139. _The Mass of the Sun._--The sun is much less dense than the earth.
The mass of the sun is only 330,000 times that of the earth, and its
density only about a fourth that of the earth.

    To find the mass of the sun, we first ascertain the distance the
    earth would draw the moon towards itself in a given time, were the
    moon at the distance of the sun, and then form the proportion: as
    the distance the earth would draw the moon towards itself is to the
    distance that the sun draws the earth towards itself in the same
    time, so is the mass of the earth to the mass of the sun.

Although the mass of the sun is over three hundred thousand times that
of the earth, the pull of gravity at the surface of the sun is only
about twenty-eight times as great as at the surface of the earth. This
is because the distance from the surface of the sun to its centre is
much greater than from the surface to the centre of the earth.

[Illustration: Fig. 155.]

140. _Size of the Sun Compared with that of the Planets._--The size of
the sun compared with that of the larger planets is shown in Fig. 155.
The mass of the sun is more than seven hundred and fifty times that of
all of the planets and moons in the solar system. In Fig. 156 is shown
the apparent size of the sun as seen from the different planets. The
apparent diameter of the sun decreases as the distance from it
increases, and the disk of the sun decreases as the square of the
distance from it increases.

[Illustration: Fig. 156.]

141. _The Distance of the Sun._--The mean distance of the sun from the
earth is about 92,800,000 miles. Owing to the eccentricity of the
earth's orbit, the distance of the sun varies somewhat; being about
3,000,000 miles less in January, when the earth is at perihelion, than
in June, when the earth is at aphelion.

    "But, though the distance of the sun can easily be stated in
    figures, it is not possible to give any real idea of a space so
    enormous: it is quite beyond our power of conception. If one were to
    try to walk such a distance, supposing that he could walk four miles
    an hour, and keep it up for ten hours every day, it would take
    sixty-eight years and a half to make a single million of miles, and
    more than sixty-three hundred years to traverse the whole.

    "If some celestial railway could be imagined, the journey to the
    sun, even if our trains ran sixty miles an hour day and night and
    without a stop, would require over a hundred and seventy-five years.
    Sensation, even, would not travel so far in a human lifetime. To
    borrow the curious illustration of Professor Mendenhall, if we could
    imagine an infant with an arm long enough to enable him to touch the
    sun and burn himself, he would die of old age before the pain could
    reach him; since, according to the experiments of Helmholtz and
    others, a nervous shock is communicated only at the rate of about a
    hundred feet per second, or 1,637 miles a day, and would need more
    than a hundred and fifty years to make the journey. Sound would do
    it in about fourteen years, if it could be transmitted through
    celestial space; and a cannon-ball in about nine, if it were to move
    uniformly with the same speed as when it left the muzzle of the gun.
    If the earth could be suddenly stopped in her orbit, and allowed to
    fall unobstructed toward the sun, under the accelerating influence
    of his attraction, she would reach the centre in about four months.
    I have said if she could be stopped; but such is the compass of her
    orbit, that, to make its circuit in a year, she has to move nearly
    nineteen miles a second, or more than fifty times faster than the
    swiftest rifle-ball; and, in moving twenty miles, her path deviates
    from perfect straightness by less than an eighth of an inch. And
    yet, over all the circumference of this tremendous orbit, the sun
    exercises his dominion, and every pulsation of his surface receives
    its response from the subject earth." (Professor C. A. Young: The
    Sun.)

    142. _Method of Finding the Sun's Distance._--There are several
    methods of finding the sun's distance. The simplest method is that
    of finding the actual distance of one of the nearer planets by
    observing its displacement in the sky as seen from widely separated
    points on the earth. As the _relative_ distances of the planets from
    each other and from the sun are well known, we can easily deduce the
    actual distance of the sun if we can find that of any of the
    planets. The two planets usually chosen for this method are Mars and
    Venus.

    (1) The displacement of Mars in the sky, as seen from two
    observatories which differ considerably in latitude, is, of course,
    greatest when Mars is nearest the earth. Now, it is evident than
    Mars will be nearer the earth when in opposition than when in any
    other part of its orbit; and the planet will be least distant from
    the earth when it is at its perihelion point, and the earth is at
    its aphelion point, at the time of opposition. This method, then,
    can be used to the best advantage, when, at the time of opposition,
    Mars is near its perihelion, and the earth near its aphelion. These
    favorable oppositions occur about once in fifteen years, and the
    last one was in 1877.

[Illustration: Fig. 157.]

    Suppose two observers situated at _N'_ and _S'_ (Fig. 157), near the
    poles of the earth. The one at _N'_ would see Mars in the sky at
    _N_, and the one at _S'_ would see it at _S_. The displacement would
    be the angle _NMS_. Each observer measures carefully the distance of
    Mars from the same fixed star near it. The difference of these
    distances gives the displacement of the planet, or the angle _NMS_.
    These observations were made with the greatest care in 1877.

    (2) Venus is nearest the earth at the time of inferior conjunction;
    but it can then be seen only in the daytime. It is, therefore,
    impossible to ascertain the displacement of Venus, as seen from
    different stations, by comparing her distances from a fixed star.
    Occasionally, at the time of inferior conjunction, Venus passes
    directly across the sun's disk. The last of these _transits_ of
    Venus occurred in 1874, and the next will occur in 1882. It will
    then be over a hundred years before another will occur.

[Illustration: Fig. 158.]

    Suppose two observers, _A_ and _B_ (Fig. 158), near the poles of the
    earth at the time of a transit of Venus. The observer at _A_ would
    see Venus crossing the sun at _V_{2}_, and the one at _B_ would see
    it crossing at _V_{1}_. Any observation made upon Venus, which would
    give the distance and direction of Venus from the centre of the sun,
    as seen from each station, would enable us to calculate the angular
    distance between the two chords described across the sun. This, of
    course, would give the displacement of Venus on the sun's disk. This
    method was first employed at the last transits of Venus which
    occurred before 1874; namely, those of 1761 and 1769.

    There are three methods of observation employed to ascertain the
    apparent direction and distance of Venus from the centre of the sun,
    called respectively the _contact method_, the _micrometric method_,
    and the _photographic method_.

    (_a_) In the _contact_ method, the observation consists in noting
    the exact time when Venus crosses the sun's limb. To ascertain this
    it is necessary to observe the exact time of external and internal
    contact. This observation, though apparently simple, is really very
    difficult. With reference to this method Professor Young says,--

    "The difficulties depend in part upon the imperfections of optical
    instruments and the human eye, partly upon the essential nature of
    light leading to what is known as diffraction, and partly upon the
    action of the planet's atmosphere. The two first-named causes
    produce what is called irradiation, and operate to make the apparent
    diameter of the planet, as seen on the solar disk, smaller than it
    really is; smaller, too, by an amount which varies with the size of
    the telescope, the perfection of its lenses, and the tint and
    brightness of the sun's image. The edge of the planet's image is
    also rendered slightly hazy and indistinct.

[Illustration: Fig. 159.]

    "The planet's atmosphere also causes its disk to be surrounded by a
    narrow ring of light, which becomes visible long before the planet
    touches the sun, and, at the moment of internal contact, produces an
    appearance, of which the accompanying figure is intended to give an
    idea, though on an exaggerated scale. The planet moves so slowly as
    to occupy more than twenty minutes in crossing the sun's limb; so
    that even if the planet's edge were perfectly sharp and definite,
    and the sun's limb undistorted, it would be very difficult to
    determine the precise second at which contact occurs. But, as things
    are, observers with precisely similar telescopes, and side by side,
    often differ from each other five or six seconds; and, where the
    telescopes are not similar, the differences and uncertainties are
    much greater.... Astronomers, therefore, at present are pretty much
    agreed that such observations can be of little value in removing the
    remaining uncertainty of the parallax, and are disposed to put more
    reliance upon the micrometric and photographic methods, which are
    free from these peculiar difficulties, though, of course, beset with
    others, which, however, it is hoped will prove less formidable."

    (_b_) Of the _micrometric_ method, as employed at the last transit,
    Professor Young speaks as follows:--

    "The micrometric method requires the use of a heliometer,--an
    instrument common only in Germany, and requiring much skill and
    practice in its use in order to obtain with it accurate measures. At
    the late transit, a single English party, two or three of the
    Russian parties, and all five of the German, were equipped with
    these instruments; and at some of the stations extensive series of
    measures were made. None of the results, however, have appeared as
    yet; so that it is impossible to say how greatly, if at all, this
    method will have the advantage in precision over the contact
    observations."

    (_c_) The following observations, with reference to the
    _photographic_ method, are also taken from Professor Young:--

    "The Americans and French placed their main reliance upon the
    photographic method, while the English and Germans also provided for
    its use to a certain extent. The great advantage of this method is,
    that it makes it possible to perform the necessary measurements
    (upon whose accuracy every thing depends) at leisure after the
    transit, without hurry, and with all possible precautions. The
    field-work consists merely in obtaining as many and as good pictures
    as possible. A principal objection to the method lies in the
    difficulty of obtaining good pictures, i.e., pictures free from
    distortion, and so distinct and sharp as to bear high magnifying
    power in the microscopic apparatus used for their measurement. The
    most serious difficulty, however, is involved in the accurate
    determination of the scale of the picture; that is, of the number of
    seconds of arc corresponding to a linear inch upon the plate.
    Besides this, we must know the exact Greenwich time at which each
    picture is taken, and it is also extremely desirable that the
    _orientation_ of the picture should be accurately determined; that
    is, the north and south, the east and west points of the solar image
    on the finished plate. There has been a good deal of anxiety lest
    the image, however accurate and sharp when first produced, should
    alter, in course of time, through the contraction of the collodion
    film on the glass plate; but the experiments of Rutherfurd, Huggins,
    and Paschen, seem to show that this danger is imaginary.... The
    Americans placed the photographic telescope exactly in line with a
    meridian instrument, and so determined, with the extremest
    precision, the direction in which it was pointed. Knowing this and
    the time at which any picture was taken, it becomes possible, with
    the help of the plumb-line image, to determine precisely the
    orientation of the picture,--an advantage possessed by the American
    pictures alone, and making their value nearly twice as great as
    otherwise it would have been.

    "The figure below is a representation of one of the American
    photographs reduced about one-half. _V_ is the image of Venus,
    which, on the actual plate, is about a seventh of an inch in
    diameter; _aa'_ is the image of the plumb-line. The centre of the
    reticle is marked with a cross."

[Illustration: Fig. 160.]

    The English photographs proved to be of little value, and the
    results of the measurements and calculations upon the American
    pictures have not yet been published. There is a growing
    apprehension that no photographic method can be relied upon.

The most recent determinations by various methods indicate that the
sun's distance is such that his parallax is about eighty-eight seconds.
This would make the linear value of a second at the surface of the sun
about four hundred and fifty miles.

[Illustration: Plate 1.]


            II. PHYSICAL AND CHEMICAL CONDITION OF THE SUN.


                     Physical Condition of the Sun.


143. _The Sun Composed mainly of Gas._--It is now generally believed
that the sun is mainly a ball of gas, or vapor, powerfully condensed at
the centre by the weight of the superincumbent mass, but kept from
liquefying by its exceedingly high temperature.

The gaseous interior of the sun is surrounded by a layer of luminous
clouds, which constitutes its visible surface, and which is called its
_photosphere_. Here and there in the photosphere are seen dark _spots_,
which often attain an immense magnitude.

These clouds float in the _solar atmosphere_, which extends some
distance beyond them.

The luminous surface of the sun is surrounded by a _rose-colored_
stratum of gaseous matter, called the _chromosphere_. Here and there
great masses of this chromospheric matter rise high above the general
level. These masses are called _prominences_.

Outside of the chromosphere is the _corona_, an irregular halo of faint,
pearly light, mainly composed of filaments and streamers, which radiate
from the sun to enormous distances, often more than a million of miles.

In Fig. 161 is shown a section of the sun, according to Professor Young.

The accompanying lithographic plate gives a general view of the
photosphere with its spots, and of the chromosphere and its prominences.

144. _The Temperature of the Sun._--Those who have investigated the
subject of the temperature of the sun have come to very different
conclusions; some placing it as high as four million degrees Fahrenheit,
and others as low as ten thousand degrees. Professor Young thinks that
Rosetti's estimate of eighteen thousand degrees as the _effective
temperature_ of the sun's surface is probably not far from correct. By
this is meant the temperature that a uniform surface of lampblack of the
size of the sun must have in order to radiate as much heat as the sun
does. The most intense artificial heat does not exceed four thousand
degrees Fahrenheit.

[Illustration: Fig. 161.]

145. _The Amount of Heat Radiated by the Sun._--A unit of heat is the
amount of heat required to raise a pound of water one degree in
temperature. It takes about a hundred and forty-three units of heat to
melt a pound of ice without changing its temperature. A cubic foot of
ice weighs about fifty-seven pounds. According to Sir William Herschel,
were all the heat radiated by the sun concentrated on a cylinder of ice
forty-five miles in diameter, it would melt it off at the rate of about
a hundred and ninety thousand miles a second.

Professor Young gives the following illustration of the energy of solar
radiation: "If we could build up a solid column of ice from the earth to
the sun, two miles and a quarter in diameter, spanning the inconceivable
abyss of ninety-three million miles, and if then the sun should
concentrate his power upon it, it would dissolve and melt, not in an
hour, nor a minute, but in a single second. One swing of the pendulum,
and it would be water; seven more, and it would be dissipated in vapor."

[Illustration: Fig. 162.]

This heat would be sufficient to melt a layer of ice nearly fifty feet
thick all around the sun in a minute. To develop this heat would require
the hourly consumption of a layer of anthracite coal, more than sixteen
feet thick, over the entire surface of the sun; and the _mechanical
equivalent_ of this heat is about ten thousand horse-power on every
square foot of the sun's surface.

146. _The Brightness of the Sun's Surface._--The sun's surface is a
hundred and ninety thousand times as bright as a candle-flame, a hundred
and forty-six times as bright as the calcium-light, and about three
times and a half as bright as the voltaic arc.

The sun's disk is much less bright near the margin than near the centre,
a point on the limb of the sun being only about a fourth as bright as
one near the centre of the disk. This diminution of brightness towards
the margin of the disk is due to the increase in the absorption of the
solar atmosphere as we pass from the centre towards the margin of the
sun's disk; and this increased absorption is due to the fact, that the
rays which reach us from near the margin have to traverse a much greater
thickness of the solar atmosphere than those which reach us from the
centre of the disk. This will be evident from Fig. 162, in which the
arrows mark the paths of rays from different parts of the solar disk.


                           The Spectroscope.


[Illustration: Fig. 163.]

147. _The Spectroscope as an Astronomical Instrument._--The
_spectroscope_ is now continually employed in the study of the physical
condition and chemical constitution of the sun and of the other heavenly
bodies. It has become almost as indispensable to the astronomer as the
telescope.

148. _The Dispersion Spectroscope._--The essential parts of the
_dispersion_ spectroscope are shown in Fig. 163. These are the
_collimator tube_, the _prism_, and the _telescope_. The collimator tube
has a narrow slit at one end, through which the light to be examined is
admitted, and somewhere within the tube a lens for condensing the light.
The light is dispersed on passing through the prism: it then passes
through the objective of the telescope, and forms within the tube an
image of the spectrum, which is examined by means of the eye-piece. The
power of the spectroscope is increased by increasing the number of
prisms, which are arranged so that the light shall pass through one
after another in succession. Such an arrangement of prisms is shown in
Fig. 164. One end of the collimator tube is seen at the left, and one
end of the telescope at the right. Sometimes the prisms are made long,
and the light is sent twice through the same train of prisms, once
through the lower, and once through the upper, half of the prisms. This
is accomplished by placing a rectangular prism against the last prism of
the train, as shown in Fig. 165.

[Illustration: Fig. 164.]

[Illustration: Fig. 165.]

149. _The Micrometer Scale._--Various devices are employed to obtain an
image of a micrometer scale in the tube of the telescope beside that of
the spectrum.

[Illustration: Fig. 166.]

One of the simplest of these methods is shown in Fig. 166. _A_ is the
telescope, _B_ the collimator, and _C_ the micrometer tube. The opening
at the outer end of _C_ contains a piece of glass which has a micrometer
scale marked upon it. The light from the candle shines through this
glass, falls upon the surface of the prism _P_, and is thence reflected
into the telescope, where it forms an enlarged image of the micrometer
scale alongside the image of the spectrum.

[Illustration: Fig. 167.]

150. _The Comparison of Spectra._--In order to compare two spectra, it
is desirable to be able to see them side by side in the telescope. The
images of two spectra may be obtained side by side in the telescope tube
by the use of a little rectangular prism, which covers one-half of the
slit of the collimator tube, as shown in Fig. 167. The light from one
source is admitted directly through the uncovered half of the slit,
while the light from the other source is sent through the covered
portion of the slit by reflection from the surface of the rectangular
prism. This arrangement and its action will be readily understood from
Fig. 167.

[Illustration: Fig. 168.]

151. _Direct-Vision Spectroscope._--A beam of light may be dispersed,
without any ultimate deflection from its course, by combining prisms of
crown and flint glass with equal refractive, but unequal dispersive
powers. Such a combination of prisms is called a _direct-vision_
combination. One of three prisms is shown in Fig. 168, and one of five
prisms in Fig. 169.

[Illustration: Fig. 169.]

[Illustration: Fig. 170.]

A _direct-vision spectroscope_ (Fig. 170) is one in which a
direct-vision combination of prisms is employed. _C_ is the collimator
tube, _P_ the train of prisms, _F_ the telescope, and _r_ the comparison
prism.

[Illustration: Fig. 171.]

152. _The Telespectroscope._--The spectroscope, when used for
astronomical work, is usually combined with a telescope. The compound
instrument is called a _telespectroscope_. The spectroscope is mounted
at the end of the telescope in such a way that the image formed by the
object-glass of the telescope falls upon the slit at the end of the
collimator tube. A telespectroscope of small dispersive power is shown
in Fig. 171; _a_ being the object-glass of the telescope, _cc_ the tube
of the telescope, and _e_ the comparison prism at the end of the
collimator tube. A more powerful instrument is shown in Fig. 172. _A_ is
the telescope, _C_ the collimator tube of the spectroscope, _P_ the
train of prisms, and _E_ the telescope tube. Fig. 173 shows a still more
powerful spectroscope attached to the great Newall refractor (18).

[Illustration: Fig. 172.]

[Illustration: Fig. 173.]

153. _The Diffraction Spectroscope._--A _diffraction_ spectroscope is
one in which the spectrum is produced by reflection of the light from a
finely ruled surface, or _grating_, as it is called, instead of by
dispersion in passing through a prism. The essential parts of this
instrument are shown in Fig 174. This spectroscope may be attached to
the telescope in the same manner as the dispersion spectroscope. When
the spectroscope is thus used, the eye-piece of the telescope is
removed.

[Illustration: Fig. 174.]


                                Spectra.


154. _Continuous Spectra._--Light from an incandescent solid or liquid
which has suffered no absorption in the medium which it has traversed
gives a spectrum consisting of a continuous colored band, in which the
colors, from the red to the violet, pass gradually and imperceptibly
into one another. The spectrum is entirely free from either light or
dark lines, and is called a _continuous spectrum_.

155. _Bright-Lined Spectra._--Light from a luminous gas or vapor gives a
spectrum composed of bright lines separated by dark spaces, and known as
a _bright-lined spectrum_. It has been found that the lines in the
spectrum of a substance in the state of a gas or vapor are the most
characteristic thing about the substance, since no two vapors give
exactly the same lines: hence, when we have once become acquainted with
the bright-lined spectrum of any substance, we can ever after recognize
that substance by the spectrum of its luminous vapor. Even when several
substances are mixed, they may all be recognized by the bright-lined
spectrum of the mixture, since the lines of all the substances will be
present in the spectrum of the mixture. This method of identifying
substances by their spectra is called _spectrum analysis_.

The bright-lined spectra of several substances are given in the
frontispiece. The number of lines in the spectra of the elements varies
greatly. The spectrum of sodium is one of the simplest, while that of
iron is one of the most complex. The latter contains over six hundred
lines. Though no two vapors give identical spectra, there are many cases
in which one or more of the spectral lines of one element coincide in
position with lines of other elements.

    156. _Methods of rendering Gases and Vapors Luminous._--In order to
    study the spectra of vapors and gases it is necessary to have some
    means of converting solids and liquids into vapor, and also of
    rendering the vapors and gases luminous. There are four methods of
    obtaining luminous vapors and gases in common use.

[Illustration: Fig. 175.]

(1) _By means of the Bunsen Flame._--This is a very hot but an almost
non-luminous flame. If any readily volatilized substance, such as the
compounds of sodium, calcium, strontium, etc., is introduced into this
flame on a fine platinum wire, it is volatilized in the flame, and its
vapor is rendered luminous, giving the flame its own peculiar color. The
flame thus colored may be examined by the spectroscope. The arrangement
of the flame is shown in Fig. 175.

[Illustration: Fig. 176.]

(2) _By means of the Voltaic Arc._--An electric lamp is shown in Fig.
176. When this lamp is to be used for obtaining luminous vapors, the
lower carbon is made larger than the upper one, and hollowed out at the
top into a little cup. The substance to be volatilized is placed in this
cup, and the current is allowed to pass. The heat of the voltaic arc is
much more intense than that of the Bunsen flame: hence substances that
cannot be volatilized in the flame are readily volatilized in the arc,
and the vapor formed is raised to a very high temperature.

(3) _By means of the Spark from an Induction Coil._--The arrangement of
the coil for obtaining luminous vapors is shown in Fig. 177.

[Illustration: Fig. 177.]

The terminals of the coil between which the spark is to pass are brought
quite close together. When we wish to vaporize any metal, as iron, the
terminals are made of iron. On the passage of the spark, a little of the
iron at the ends of the terminals is evaporated; and the vapor is
rendered luminous in the space traversed by the spark. A condenser is
usually placed in the circuit. With the coil, the temperature may be
varied at pleasure; and the vapor may be raised even to a higher
temperature than with the electric lamp. To obtain a low temperature,
the coil is used without the condenser. By using a larger and larger
condenser, the temperature may be raised higher and higher.

By means of the induction coil we may also heat gases to incandescence.
It is only necessary to allow the spark to pass through a space filled
with the gas.

[Illustration: Fig. 178.]

(4) _By means of a Vacuum Tube._--The form of the vacuum tube commonly
used for this purpose is shown in Fig. 178. The gas to be examined, and
which is contained in the tube, has very slight density: but upon the
passage of the discharge from an induction coil or a Holtz machine,
through the tube, the gas in the capillary part of the tube becomes
heated to a high temperature, and is then quite brilliant.

157. _Reversed Spectra._--If the light from an incandescent cylinder of
lime, or from the incandescent point of an electric lamp, is allowed to
pass through luminous sodium vapor, and is then examined with a
spectroscope, the spectrum will be found to be a bright spectrum crossed
by a single _dark_ line in the position of the yellow line of the sodium
vapor. The spectrum of sodium vapor is _reversed_, its bright lines
becoming dark and its dark spaces bright. With a spectroscope of any
considerable power, the yellow line of sodium vapor is resolved into a
double line. With a spectroscope of the same power, the dark sodium line
of the reversed spectrum is seen to be a double line.

It is found to be generally true, that the spectrum of the light from an
incandescent solid or liquid which has passed _through a luminous vapor_
on its way to the spectroscope is made up of a bright ground crossed by
dark lines; there being a dark line for every bright line that the vapor
alone would give.

158. _Explanation of Reversed Spectra._--It has been found that gases
absorb and quench rays of the same degree of refrangibility as those
which they themselves emit, and no others. When a solid is shining
through a luminous vapor, this absorbs and quenches those rays from the
solid which have the same degrees of refrangibility as those which it is
itself emitting: hence the lines of the spectrum receive light from the
vapor alone, while the spaces between the lines receive light from the
solid. Now, solids and liquids, when heated to incandescence, give a
very much brighter light than vapors and gases at the same temperature:
hence the lines of a reversed spectrum, though receiving light from the
vapor or gas, appear dark by contrast.

159. _Effect of Increasing the Power of the Spectroscope upon the
Brilliancy of a Spectrum._--An increase in the power of a spectroscope
diminishes the brilliancy of a _continuous_ spectrum, since it makes the
colored band longer, and therefore spreads the light out over a greater
extent of surface; but, in the case of a _bright-lined_ spectrum, an
increase of power in the spectroscope produces scarcely any alteration
in the brilliancy of the lines, since it merely separates the lines
farther without making the lines themselves any wider. In the case of a
_reversed_ spectrum, an increase of power in the spectroscope dilutes
the light in the spaces between the lines without diluting that of the
lines: hence lines which appear dark in a spectroscope of slight
dispersive power may appear bright in an instrument of great dispersive
power.

160. _Change of the Spectrum with the Density of the Luminous
Vapor._--It has been found, that, as the density of a luminous vapor is
diminished, the lines in its spectrum become fewer and fewer, till they
are finally reduced to one. On the other hand, an increase of density
causes new lines to appear in the spectrum, and the old lines to become
thicker.

161. _Change of the Spectrum with the Temperature of the Luminous
Vapor._--It has also been found that the appearance of a bright-lined
spectrum changes considerably with the temperature of the luminous
vapor. In some cases, an increase of temperature changes the relative
intensities of the lines; in other cases, it causes new lines to appear,
and old lines to disappear.

In the case of a compound vapor, an increase of temperature causes the
colored bands (which are peculiar to the spectrum of the compound) to
disappear, and to be replaced by the spectral lines of the elements of
which the compound is made up. The heat appears to _dissociate_ the
compound; that is, to resolve it into its constituent elements. In this
case, each elementary vapor would give its own spectral lines. As the
compound is not completely dissociated at once, it is possible, of
course, for one or more of the spectral lines of the elementary vapors
to co-exist in the spectrum with the bands of the compound.

It has been found, that, in some cases, the spectra of the elementary
gases change with the temperature of the gas; and Lockyer thinks he has
discovered conclusive evidence, in the spectra of the sun and stars,
that many of the substances regarded as elementary are really resolved
into simpler substances by the intense heat of the sun; in other words,
that our so-called elements are really compounds.


                   Chemical Constitution of the Sun.


162. _The Solar Spectrum._--The solar spectrum is crossed transversely
by a great number of fine dark lines, and hence it belongs to the class
of _reversed_ spectra.

These lines were first studied and mapped by Fraunhofer, and from him
they have been called _Fraunhofer's lines_.

[Illustration: Fig. 179.]

    A reduced copy of Fraunhofer's map is shown in Fig. 179. A few of
    the most prominent of the dark solar lines are designated by the
    letters of the alphabet. The other lines are usually designated by
    the numbers at which they are found on the scale which accompanies
    the map. This scale is usually drawn at the top of the map, as will
    be seen in some of the following diagrams. The two most elaborate
    maps of the solar spectrum are those of Kirchhoff and Angström. The
    scale on Kirchhoff's map is an arbitrary one, while that of Angström
    is based upon the wave-lengths of the rays of light which would fall
    upon the lines in the spectrum.

[Illustration: Fig. 180.]

    The appearance of the spectrum varies greatly with the power of the
    spectroscope employed. Fig. 180 shows a portion of the spectrum as
    it appears in a spectroscope of a single prism: while Fig. 181 shows
    the _b_ group of lines alone, as they appear in a powerful
    diffraction spectroscope.

[Illustration: Fig. 181.]

163. _The Telluric Lines._--There are many lines of the solar spectrum
which vary considerably in intensity as the sun passes from the horizon
to the meridian, being most intense when the sun is nearest the horizon,
and when his rays are obliged to pass through the greatest depth of the
earth's atmosphere. These lines are of atmospheric origin, and are due
to the absorption of the aqueous vapor in our atmosphere. They are the
same lines that are obtained when a candle or other artificial light is
examined with a spectroscope through a long tube filled with steam.
Since these lines are due to the absorption of our own atmosphere, they
are called _telluric lines_. A map of these lines is shown in Fig. 182.

[Illustration: Fig. 182.]

164. _The Solar Lines._--After deducting the telluric lines, the
remaining lines of the solar spectrum are of solar origin. They must be
due to absorption which takes place in the sun's atmosphere. They are,
in fact, the reversed spectra of the elements which exist in the solar
atmosphere in the state of vapor: hence we conclude that the luminous
surface of the sun is surrounded with an atmosphere of luminous vapors.
The temperature of this atmosphere, at least near the surface of the
sun, must be sufficient to enable all the elements known on the earth to
exist in it as vapors.

[Illustration: Fig. 183.]

165. _Chemical Constitution of the Sun's Atmosphere._--To find whether
any element which exists on the earth is present in the solar
atmosphere, we have merely to ascertain whether the bright lines of its
gaseous spectrum are matched by dark lines in the solar spectrum when
the two spectra are placed side by side. In Fig. 183, we have in No. 1 a
portion of the red end of the solar spectra, and in No. 2 the spectrum
of sodium vapor, both as obtained in the same spectroscope by means of
the comparison prism. It will be seen that the double sodium line is
exactly matched by a double dark line of the solar spectrum: hence we
conclude that sodium vapor is present in the sun's atmosphere. Fig. 184
shows the matching of a great number of the bright lines of iron vapor
by dark lines in the solar spectrum. This matching of the iron lines
establishes the fact that iron vapor is present in the solar atmosphere.

[Illustration: Fig. 184.]

    The following table (given by Professor Young) contains a list of
    all the elements which have, up to the present time, been detected
    with certainty in the sun's atmosphere. It also gives the number of
    bright lines in the spectrum of each element, and the number of
    those lines which have been matched by dark lines in the solar
    spectrum:--

            Elements.      Bright Lines Reversed. Observer.
                           Lines.

            1. Iron           600             460 Kirchhoff.

            2. Titanium       206             118 Thalen.

            3. Calcium         89              75 Kirchhoff.

            4. Manganese       75              57 Angström.

            5. Nickel          51              33 Kirchhoff.

            6. Cobalt          86              19 Thalen.

            7. Chromium        71              18 Kirchhoff.

            8. Barium          26              11 Kirchhoff.

            9. Sodium           9               9 Kirchhoff.

            10. Magnesium       7               7 Kirchhoff.

            11. Copper?        15              7? Kirchhoff.

            12. Hydrogen        5               5 Angström.

            13. Palladium      29               5 Lockyer.

            14. Vanadium       54               4 Lockyer.

            15. Molybdenum     27               4 Lockyer.

            16. Strontium      74               4 Lockyer.

            17. Lead           41               3 Lockyer.

            18. Uranium        21               3 Lockyer.

            19. Aluminium      14               2 Angström.

            20. Cerium         64               2 Lockyer.

            21. Cadmium        20               2 Lockyer.

            22. Oxygen a       42     12 ± bright H. Draper.

            Oxygen b            4              4? Schuster.

    In addition to the above elements, it is probable that several other
    elements are present in the sun's atmosphere; since at least one of
    their bright lines has been found to coincide with dark lines of the
    solar spectrum. There are, however, a large number of elements, no
    traces of which have yet been detected; and, in the cases of the
    elements whose presence in the solar atmosphere has been
    established, the matching of the lines is far from complete in the
    majority of the cases, as will be seen from the above table. This
    want of complete coincidence of the lines is undoubtedly due to the
    very high temperature of the solar atmosphere. We have already seen
    that the lines of the spectrum change with the temperature; and, as
    the temperature of the sun is far higher than any that we can
    produce by artificial means, we might reasonably expect that it
    would cause the disappearance from the spectrum of many lines which
    we find to be present at our highest temperature.

    Lockyer maintains that the reason why no trace of the spectral lines
    of certain of our so-called elements is found in the solar
    atmosphere is, that these substances are not really elementary, and
    that the intense heat of the sun resolves them into simpler
    constituents.


                   Motion at the Surface of the Sun.


166. _Change of Pitch caused by Motion of Sounding Body._--When a
sounding body is moving rapidly towards us, the pitch of its note
becomes somewhat higher than when the body is stationary; and, when such
a body is moving rapidly from us, the pitch of its note is lowered
somewhat. We have a good illustration of this change of pitch at a
country railway station on the passage of an express-train. The pitch of
the locomotive whistle is considerably higher when the train is
approaching the station than when it is leaving it.

167. _Explanation of the Change of Pitch produced by Motion._--The pitch
of sound depends upon the rapidity with which the pulsations of sound
beat upon the drum of the ear. The more rapidly the pulsations follow
each other, the higher is the pitch: hence the shorter the sound-waves
(provided the sound is all the while travelling at the same rate), the
higher the pitch of the sound. Any thing, then, which tends to shorten
the waves of sound tends also to raise its pitch, and any thing which
tends to lengthen these waves tends to lower its pitch.

When a sounding body is moving rapidly forward, the sound-waves are
crowded together a little, and therefore shortened; when it is moving
backward, the sound-waves are drawn out, or lengthened a little.

    The effect of the motion of a sounding body upon the length of its
    sonorous waves will be readily seen from the following illustration:
    Suppose a number of persons stationed at equal intervals in a line
    on a long platform capable of moving backward and forward. Suppose
    the men are four feet apart, and all walking forward at the same
    rate, and that the platform is stationary, and that, as the men
    leave the platform, they keep on walking at the same rate: the men
    will evidently be four feet apart in the line in front of the
    platform, as well as on it. Suppose next, that the platform is
    moving forward at the rate of one foot in the interval between two
    men's leaving the platform, and that the men continue to walk as
    before: it is evident that the men will then be three feet apart in
    the line after they have left the platform. The forward motion of
    the platform has the effect of crowding the men together a little.
    Were the platform moving backward at the same rate, the men would be
    five feet apart after they had left the platform. The backward
    motion of the platform has the effect of separating the men from one
    another.

    The distance between the men in this illustration corresponds to the
    length of the sound-wave, or the distance between its two ends. Were
    a person to stand beside the line, and count the men that passed him
    in the three cases given above, he would find that more persons
    would pass him in the same time when the platform is moving forward
    than when it is stationary, and fewer persons would pass him in the
    same time when the platform is moving backward than when it is
    stationary. In the same way, when a sounding body is moving rapidly
    forward, the sound-waves beat more rapidly upon the ear of a person
    who is standing still than when the body is at rest, and less
    rapidly when the sounding body is moving rapidly backward.

    Were the platform stationary, and were the person who is counting
    the men to be walking along the line, either towards or away from
    the platform, the effect upon the number of men passing him in a
    given time would be precisely the same as it would be were the
    person stationary, and the platform moving either towards or away
    from him at the same rate. So the change in the rapidity with which
    pulsations of sound beat upon the ear is precisely the same whether
    the ear is stationary and the sounding body moving, or the sounding
    body is stationary and the ear moving.

168. _Change of Refrangibility due to the Motion of a Luminous
Body._--Refrangibility in light corresponds to pitch in sound, and
depends upon the length of the luminous waves. The shorter the luminous
waves, the greater the refrangibility of the waves. Very rapid motion of
a luminous body has the same effect upon the length of the luminous
waves that motion of a sounding body has upon the length of the sonorous
waves. When a luminous body is moving very rapidly towards us, its
luminous waves are shortened a little, and its light becomes a little
more refrangible; when the luminous body is moving rapidly from us, its
luminous waves are lengthened a little, and its light becomes a little
less refrangible.

[Illustration: Fig. 185.]

169. _Displacement of Spectral Lines._--In examining the spectra of the
stars, we often find that certain of the dark lines are _displaced_
somewhat, either towards the red or the violet end of the spectrum. As
the dark lines are in the same position as the bright lines of the
absorbing vapor would be, a displacement of the lines towards the red
end of the spectrum indicates a lowering of the refrangibility of the
rays, due to a motion of the luminous vapor away from us; and a
displacement of the lines towards the violet end of the spectrum
indicates an increase of refrangibility, due to a motion of the luminous
vapor towards us. From the amount of the displacement of the lines, it
is possible to calculate the velocity at which the luminous gas is
moving. In Fig. 185 is shown the displacement of the _F_ line in the
spectrum of Sirius. This is one of the hydrogen lines. _RV_ is the
spectrum, _R_ being the red, and _V_ the violet end. The long vertical
line is the bright _F_ line of hydrogen, and the short dark line to the
left of it is the position of the _F_ line in the spectrum of Sirius. It
is seen that this line is displaced somewhat towards the red end of the
spectrum. This indicates that Sirius must be moving from us; and the
amount of the displacement indicates that the star must be moving at the
rate of some twenty-five or thirty miles a second.

[Illustration: Fig. 186.]

170. _Contortion of Lines on the Disk of the Sun._--Certain of the dark
lines seen on the centre of the sun's disk often appear more or less
distorted, as shown in Fig. 186, which represents the contortion of the
hydrogen line as seen at various times. 1 and 2 indicate a rapid motion
of hydrogen away from us, or a _down-rush_ at the sun; 3 and 4 (in which
the line at the centre is dark on one side, and bent towards the red end
of the spectrum, and bright on the other side with a distortion towards
the violet end of the spectrum) indicate a _down-rush_ of _cool_
hydrogen side by side with an _up-rush_ of _hot and bright_ hydrogen; 5
indicates local _down-rushes_ associated with _quiescent_ hydrogen.

The contorted lines, which indicate a violently agitated state of the
sun's atmosphere, appear in the midst of other lines which indicate a
quiescent state. This is owing to the fact that the absorption which
produces the dark lines takes place at various depths in the solar
atmosphere. There may be violent commotion in the lower layers of the
sun's atmosphere, and comparative quiet in the upper layers. In this
case, the lines which are due to absorption in the lower layers would
indicate this disturbance by their contortions; while the lines produced
by absorption in the upper layers would be free from contortion.

It often happens, too, that the contortions are confined to one set of
lines of an element, while other lines of the same element are entirely
free from contortions. This is undoubtedly due to the fact that
different layers of the solar atmosphere differ greatly in temperature;
so that the same element would give one set of lines at one depth, and
another set at another depth: hence commotion in the solar atmosphere at
any particular depth would be indicated by the contortion of those lines
of the element only which are produced by the temperature at that
particular depth.

A remarkable case of contortion witnessed by Professor Young is shown in
Fig. 187. Three successive appearances of the _C_ line are shown. The
second view was taken three minutes after the first, and the third five
minutes after the second. The contortion in this case indicated a
velocity ranging from two hundred to three hundred miles a second.

[Illustration: Fig. 187.]

171. _Contortion of Lines on the Sun's Limb._--When the spectroscope is
directed to the centre of the sun's disk, the distortion of the lines
indicates only vertical motion in the sun's atmosphere; but, when the
spectroscope is directed to the limb of the sun, displacements of the
lines indicate horizontal motions in the sun's atmosphere. When a
powerful spectroscope is directed to the margin of the sun's disk, so
that the slit of the collimator tube shall be perpendicular to the sun's
limb, one or more of the dark lines on the disk are seen to be prolonged
by a bright line, as shown in Fig. 188. But this prolongation, instead
of being straight and narrow, as shown in the figure, is often widened
and distorted in various ways, as shown in Fig. 189. In the left-hand
portion of the diagram, the line is deflected towards the red end of the
spectrum; this indicates a violent wind on the sun's surface blowing
away from us. In the right-hand portion of the diagram, the line is
deflected towards the violet end of the spectrum; this indicates a
violent wind blowing towards us. In the middle portion of the figure,
the line is seen to be bent both ways; this indicates a cyclone, on one
side of which the wind would be blowing from us, and on the other side
towards us.

[Illustration: Fig. 188.]

[Illustration: Fig. 189.]

The distortions of the solar lines indicate that the wind at the surface
of the sun often blows with a velocity of _from one hundred to three
hundred miles a second_. The most violent wind known on the earth has
velocity of a hundred miles an hour.


                  III. THE PHOTOSPHERE AND SUN SPOTS.


                            The Photosphere.


[Illustration: Fig. 190.]

172. _The Granulation of the Photosphere._--When the surface of the sun
is examined with a good telescope under favorable atmospheric
conditions, it is seen to be composed of minute grains of intense
brilliancy and of irregular form, floating in a darker medium, and
arranged in streaks and groups, as shown in Fig. 190. With a rather low
power, the general effect of the surface is much like that of rough
drawing-paper, or of curdled milk seen from a little distance. With a
high power and excellent atmospheric conditions, the _grains_ are seen
to be irregular, rounded masses, some hundreds of miles in diameter,
sprinkled upon a less brilliant background, and appearing somewhat like
snow-flakes sparsely scattered over a grayish cloth. Fig. 191 is a
representation of these grains according to Secchi.

[Illustration: Fig. 191.]

With a very powerful telescope and the very best atmospheric conditions,
the grains themselves are resolved into _granules_, or little luminous
dots, not more than a hundred miles or so in diameter, which, by their
aggregation, make up the grains, just as they, in their turn, make up
the coarser masses of the solar surface. Professor Langley estimates
that these granules constitute about one-fifth of the sun's surface,
while they emit at least three-fourths of its light.

173. _Shape of the Grains._--The grains differ considerably in shape at
different times and on different parts of the sun's surface. Nasmyth, in
1861, described them as _willow-leaves_ in shape, several thousand miles
in length, but narrow and with pointed ends. He figured the surface of
the sun as a sort of basket-work formed by the interweaving of such
filaments. To others they have appeared to have the form of
_rice-grains_. On portions of the sun's disk the elementary structure is
often composed of long, narrow, blunt-ended filaments, not so much like
willow-leaves as like bits of straw lying roughly parallel to each
other,--a _thatch-straw_ formation, as it has been called. This is
specially common in the immediate neighborhood of the spots.

174. _Nature of the Grains._--The grains are, undoubtedly, incandescent
_clouds_ floating in the sun's atmosphere, and composed of partially
condensed metallic vapors, just as the clouds of our atmosphere are
composed of partially condensed aqueous vapor. Rain on the sun is
composed of white-hot drops of molten iron and other metals; and these
drops are often driven with the wind with a velocity of over a hundred
miles a second.

As to the forms of the grains, Professor Young says, "If one were to
speculate as to the explanation of the grains and thatch-straws, it
might be that the grains are the upper ends of long filaments of
luminous cloud, which, over most of the sun's surface, stand
approximately vertical, but in the neighborhood of a spot are inclined
so as to lie nearly horizontal. This is not certain, though: it may be
that the cloud-masses over the more quiet portions of the solar surface
are really, as they seem, nearly globular, while near the spots they are
drawn out into filamentary forms by atmospheric currents."

175. _Faculæ._--The _faculæ_ are irregular streaks of greater brightness
than the general surface, looking much like the flecks of foam on the
surface of a stream below a waterfall. They are sometimes from five to
twenty thousand miles in length, covering areas immensely larger than a
terrestrial continent.

These faculæ are _elevated regions_ of the solar surface, ridges and
crests of luminous matter, which rise above the general level of the
sun's surface, and protrude through the denser portions of the solar
atmosphere. When one of these passes over the edge of the sun's disk, it
can be seen to project, like a little tooth. Any elevation on the sun to
be perceptible at all must measure at least half a second of an arc, or
two hundred and twenty-five miles.

The faculæ are most numerous in the neighborhood of the spots, and much
more conspicuous near the limb of the sun than near the centre of the
disk. Fig. 192 gives the general appearance of the faculæ, and the
darkening of the limb of the sun. Near the spots, the faculæ often
undergo very rapid change of form, while elsewhere on the disk they
change rather slowly, sometimes undergoing little apparent alteration
for several days.

[Illustration: Fig. 192.]

176. _Why the Faculæ are most Conspicuous near the Limb of the
Sun._--The reason why the faculæ are most conspicuous near the limb of
the sun is this: The luminous surface of the sun is covered with an
atmosphere, which, though not very thick compared with the diameter of
the sun, is still sufficient to absorb a good deal of light. Light
coming from the centre of the sun's disk penetrates this atmosphere
under the most favorable conditions, and is but slightly reduced in
amount. The edges of the disk, on the other hand, are seen through a
much greater thickness of atmosphere; and the light is reduced by
absorption some seventy-five per cent. Suppose, now, a facula were
sufficiently elevated to penetrate quite through this atmosphere. Its
light would be undimmed by absorption on any part of the sun's disk; but
at the centre of the disk it would be seen against a background nearly
as bright as itself, while at the margin it would be seen against one
only a quarter as bright. It is evident that the light of any facula,
owing to the elevation, would be reduced less rapidly as we approach the
edge of the disk than that of the general surface of the sun, which lies
at a lower level.


                               Sun-Spots.


177. _General Appearance of Sun-Spots._--The general appearance of a
well-formed sun-spot is shown in Fig. 193. The spot consists of a very
dark central portion of irregular shape, called the _umbra_, which is
surrounded by a less dark fringe, called the _penumbra_. The penumbra is
made up, for the most part, of filaments directed radially inward.

[Illustration: Fig. 193.]

There is great variety in the details of form in different sun-spots;
but they are generally nearly circular during the middle period of their
existence. During the period of their development and of their
disappearance they are much more irregular in form.

There is nothing like a gradual shading-off of the penumbra, either
towards the umbra on the one side, or towards the photosphere on the
other. The penumbra is separated from both the umbra and the photosphere
by a sharp line of demarcation. The umbra is much brighter on the inner
than on the outer edge, and frequently the photosphere is excessively
bright at the margin of the penumbra. The brightness of the inner
penumbra seems to be due to the crowding together of the penumbral
filaments where they overhang the edge of the umbra.

There is a general antithesis between the irregularities of the outer
and inner edges of the penumbra. Where an angle of the penumbral matter
crowds in upon the umbra, it is generally matched by a corresponding
outward extension into the photosphere, and _vice versa_.

The umbra of the spot is far from being uniformly dark. Many of the
penumbral filaments terminate in little detached grains of luminous
matter; and there are also fainter veils of a substance less brilliant,
but sometimes rose-colored, which seem to float above the umbra. The
umbra itself is made up of masses of clouds which are really intensely
brilliant, and which appear dark only by contrast with the intenser
brightness of the solar surface. Among these clouds are often seen one
or more minute circular spots much darker than the rest of the umbra.
These darker portions are called _nuclei_. They seem to be the mouths of
tubular orifices penetrating to unknown depths. The faint veils
mentioned above continually melt away, and are replaced by others in
some different position. The bright granules at the tips of the
penumbral filaments seem to sink and dissolve, while fresh portions
break off to replace them. There is a continual indraught of luminous
matter over the whole extent of the penumbra.

At times, though very rarely, patches of intense brightness suddenly
break out, remain visible for a few minutes, and move over the spot with
velocities as great as a hundred miles _a second_.

The spots change their form and size quite perceptibly from day to day,
and sometimes even from hour to hour.

178. _Duration of Sun-Spots._--The average life of a sun-spot is two or
three months: the longest on record is that of a spot observed in 1840
and 1841, which lasted eighteen months. There are cases, however, where
the disappearance of a spot is very soon followed by the appearance of
another at the same point; and sometimes this alternate disappearance
and re-appearance is several times repeated. While some spots are thus
long-lived, others endure only a day or two, and sometimes only a few
hours.

179. _Groups of Spots._--The spots usually appear not singly, but in
groups. A large spot is often followed by a train of smaller ones to the
east of it, many of which are apt to be irregular in form and very
imperfect in structure, sometimes with no umbra at all, often with a
penumbra only on one side. In such cases, when any considerable change
of form or structure shows itself in the principal spot, it seems to
rush westward over the solar surface, leaving its attendants trailing
behind. When a large spot divides into two or more, as often happens,
the parts usually seem to repel each other, and fly apart with great
velocity.

180. _Size of the Spots._--The spots are sometimes of enormous size.
Groups have often been observed covering areas of more than a hundred
thousand miles square, and single spots occasionally measure from forty
to fifty thousand miles in diameter, the umbra being twenty-five or
thirty thousand miles across. A spot, however, measuring thirty thousand
miles over all, may be considered a large one. Such a spot can easily be
seen without a telescope when the brightness of the sun's surface is
reduced by clouds or nearness to the horizon, or by the use of colored
glass. During the years 1871 and 1872 spots were visible to the naked
eye for a considerable portion of the time. The largest spot yet
recorded was observed in 1858. It had a breadth of more than a hundred
and forty-three thousand miles, or nearly eighteen times the diameter of
the earth, and covered about a thirty-sixth of the whole surface of the
sun.

[Illustration: Fig. 194.]

Fig. 194 represents a group of sun-spots observed by Professor Langley,
and drawn on the same scale as the small circle in the upper left-hand
corner, which represents the surface of half of our globe.

[Illustration: Fig. 195.]

181. _The Penumbral Filaments._--Not unfrequently the penumbral
filaments are curved spirally, indicating a cyclonic action, as shown in
Fig. 195. In such cases the whole spot usually turns slowly around,
sometimes completing an entire revolution in a few days. More
frequently, however, the spiral motion lasts but a short time; and
occasionally, after continuing for a while in one direction, the motion
is reversed. Very often in large spots we observe opposite spiral
movements in different portions of the umbra, as shown in Figs. 196 and
197.

[Illustration: Fig. 196.]

Neighboring spots show no tendency to rotate in the same direction. The
number of spots in which a decided cyclonic motion (like that shown in
Fig. 198) appears is comparatively small, not exceeding two or three per
cent of the whole.

[Illustration: Fig. 197.]

[Illustration: Fig. 198.]

[Illustration: Plate 2.]

Plate II. represents a typical sun-spot as delineated by Professor
Langley. At the left-hand and upper portions of this great spot the
filaments present the ordinary appearance, while at the lower edge, and
upon the great overhanging branch, they are arranged very differently.
The feathery brush below the branch, closely resembling a frost-crystal
on a window-pane, is as rare as it is curious, and has not been
satisfactorily explained.

[Illustration: Fig. 199.]

182. _Birth and Decay of Sun-Spots._--The formation of a spot is
sometimes gradual, requiring days or even weeks for its full
development; and sometimes a single day suffices. Generally, for some
time before its appearance, there is an evident disturbance of the solar
surface, indicated especially by the presence of many brilliant faculæ,
among which _pores_, or minute black dots, are scattered. These enlarge,
and between them appear grayish patches, in which the photospheric
structure is unusually evident, as if they were caused by a dark mass
lying below a thin veil of luminous filaments. This veil seems to grow
gradually thinner, and finally breaks open, giving us at last the
complete spot with its penumbra. Some of the pores coalesce with the
principal spot, some disappear, and others form the attendant train
before described (179). The spot when once formed usually assumes a
circular form, and remains without striking change until it disappears.
As its end approaches, the surrounding photosphere seems to crowd in,
and overwhelm the penumbra. Bridges of light (Fig. 199), often much
brighter than the average of the solar surface, push across the umbra;
the arrangement of the penumbra filaments becomes confused; and, as
Secchi expresses it, the luminous matter of the photosphere seems to
tumble pell-mell into the chasm, which disappears, and leaves a
disturbed surface marked with faculæ, which, in their turn, gradually
subside.

[Illustration: Fig. 200.]

183. _Motion of Sun-Spots._--The spots have a regular motion across the
disk of the sun from east to west, occupying about twelve days in the
transit. A spot generally appears first on or near the east limb, and,
after twelve or fourteen days, disappears at the west limb. At the end
of another fourteen days, or more, it re-appears at the east limb,
unless, in the mean time, it has vanished from sight entirely. This
motion of the spots is indicated by the arrow in Fig. 200. The interval
between two successive appearances of the same spot on the eastern edge
of the sun is about twenty-seven days.

[Illustration: Fig. 201.]

184. _The Rotation of the Sun._--The spots are evidently carried around
by the rotation of the sun on its axis. It is evident, from Fig. 201,
that the sun will need to make more than a complete rotation in order to
bring a spot again upon the same part of the disk as seen from the
earth. _S_ represents the sun, and _E_ the earth. The arrows indicate
the direction of the sun's rotation. When the earth is at _E_, a spot at
_a_ would be seen at the centre of the solar disk. While the sun is
turning on its axis, the earth moves in its orbit from _E_ to _E'_:
hence the sun must make a complete rotation, and turn from _a_ to _a'_
in addition, in order to bring the spot again to the centre of the disk.
To carry the spot entirely around, and then on to _a'_, requires about
twenty-seven days. From this _synodical period_ of the spot, as it might
be called, it has been calculated that the sun must rotate on its axis
in about twenty-five days.

[Illustration: Fig. 202.]

185. _The Inclination of the Sun's Axis._--The paths described by
sun-spots across the solar disk vary with the position of the earth in
its orbit, as shown in Fig. 202. We therefore conclude that the sun's
axis is not perpendicular to the plane of the earth's orbit. The sun
rotates on its axis from west to east, and the axis leans about seven
degrees from the perpendicular to the earth's orbit.

186. _The Proper Motion of the Spots._--When the period of the sun's
rotation is deduced from the motion of spots in different solar
latitudes, there is found to be considerable variation in the results
obtained. Thus spots near the equator indicate that the sun rotates in
about twenty-five days; while those in latitude 20° indicate a period
about eighteen hours longer; and those in latitude 30° a period of
twenty-seven days and a half. Strictly speaking, the sun, as a whole,
has no single period of rotation; but different portions of its surface
perform their revolutions in different times. The equatorial regions not
only move more rapidly in miles per hour than the rest of the solar
surface, but they _complete the entire rotation in shorter time_.

[Illustration: Fig. 203.]

There appears to be a peculiar surface-drift in the equatorial regions
of the sun, the cause of which is unknown, but which gives the spots a
_proper_ motion; that is, a motion of their own, independent of the
rotation of the sun.

[Illustration: Fig. 204.]

187. _Distribution of the Sun-Spots._--The sun-spots are not distributed
uniformly over the sun's surface, but occur mainly in two zones on each
side of the equator, and between the latitudes of 10° and 30°, as shown
in Fig. 203. On and near the equator itself they are comparatively rare.
There are still fewer beyond 35° of latitude, and only a single spot has
ever been recorded more than 45° from the solar equator.

Fig. 204 shows the distribution of the sun-spots observed by Carrington
during a period of eight years. The irregular line on the left-hand side
of the figure indicates by its height the comparative frequency with
which the spots occurred in different latitudes. In Fig. 205 the same
thing is indicated by different degrees of darkness in the shading of
the belts.

[Illustration: Fig. 205.]

188. _The Periodicity of the Spots._--Careful observations of the solar
spots indicate a period of about eleven years in the spot-producing
activity of the sun. During two or three years the spots increase in
number and in size; then they begin to diminish, and reach a minimum
five or six years after the maximum. Another period of about six years
brings the return of the maximum. The intervals are, however, somewhat
irregular.

[Illustration: Fig. 206.]

Fig. 206 gives a graphic representation of the periodicity of the
sun-spots. The height of the curve shows the frequency of the sun-spots
in the years given at the bottom of the figure. It appears, from an
examination of this sun-spot curve, that the average interval from a
minimum to the next following maximum is only about four years and a
half, while that from a maximum to the next following minimum is six
years and six-tenths. The disturbance which produces the sun-spots is
developed suddenly, but dies away gradually.

189. _Connection between Sun-Spots and Terrestrial Magnetism._--The
magnetic needle does not point steadily in the same direction, but is
subject to various disturbances, some of which are regular, and others
irregular.

(1) One of the most noticeable of the regular magnetic changes is the
so-called _diurnal oscillation_. During the early part of the day the
north pole of the needle moves toward the west in our latitude,
returning to its mean position about ten P.M., and remaining nearly
stationary during the night. The extent of this oscillation in the
United States is about fifteen minutes of arc in summer, and not quite
half as much in winter; but it differs very much in different localities
and at different times, and the average diurnal oscillation in any
locality increases and decreases pretty regularly during a period of
about eleven years. The maximum and minimum of this period of magnetic
disturbance are found to coincide with the maximum and minimum of the
sun-spot period. This is shown in Fig. 206, in which the dotted lines
indicate the variations in the intensity of the magnetic disturbance.

(2) Occasionally so-called _magnetic storms_ occur, during which the
compass-needle is sometimes violently disturbed, oscillating five
degrees, or even ten degrees, within an hour or two. These storms are
generally accompanied by an aurora, and an aurora is _always_
accompanied by magnetic disturbance. A careful comparison of aurora
observations with those of sun-spots shows an almost perfect parallelism
between the curves of auroral and sun-spot frequency.

(3) A number of observations render it very probable that every intense
disturbance of the solar surface is propagated to our terrestrial
magnetism with the speed of light.

[Illustration: Fig. 207.]

Fig. 207 shows certain of the solar lines as they were observed by
Professor Young on Aug. 3, 1872. The contortions of the _F_ line
indicated an intense disturbance in the atmosphere of the sun. There
were three especially notable paroxysms in this distortion, occurring at
a quarter of nine, half-past ten, and ten minutes of twelve, A.M.

[Illustration: Fig. 208.]

Fig. 208 shows the curve of magnetic disturbance as traced at Greenwich
on the same day. It will be seen from the curve that it was a day of
general magnetic disturbance. At the times of the three paroxysms, which
are given at the bottom of the figure, it will be observed that there is
a peculiar shivering of the magnetic curve.

190. _The Spots are Depressions in the Photosphere._--This fact was
first clearly brought out by Dr. Wilson of Glasgow, in 1769, from
observations upon the penumbra of a spot in November of that year. He
found, that when the spot appeared at the eastern limb, or edge of the
sun, just moving into sight, the penumbra was well marked on the side of
the spot nearest to the edge of the disk; while on the other edge of the
spot, towards the centre of the sun, there was no penumbra visible at
all, and the umbra itself was almost hidden, as if behind a bank. When
the spot had moved a day's journey toward the centre of the disk, the
whole of the umbra came into sight, and the penumbra on the inner edge
of the spot began to be visible as a narrow line. After the spot was
well advanced upon the disk, the penumbra was of the same width all
around the spot. When the spot approached the sun's western limb, the
same phenomena were repeated, but in the inverse order. The penumbra on
the _inner_ edge of the spot narrowed much faster than that on the
outer, disappeared entirely, and finally seemed to hide from sight much
of the umbra nearly a whole day before the spot passed from view around
the limb. This is precisely what would occur (as Fig. 209 clearly shows)
if the spot were a saucer-shaped depression in the solar surface, the
bottom of the saucer corresponding to the umbra, and the sloping sides
to the penumbra.

[Illustration: Fig. 209.]

[Illustration: Fig. 210.]

191. _Sun-Spot Spectrum._--When the image of a sun-spot is thrown upon
the slit of the spectroscope, the spectrum is seen to be crossed
longitudinally by a continuous dark band, showing an increased general
absorption in the region of the sun-spot. Many of the spectral lines are
greatly thickened, as shown in Fig. 210. This thickening of the lines
shows that the absorption is taking place at a greater depth. New lines
and shadings often appear, which indicate, that, in the cooler nucleus
of the spot, certain compound vapors exist, which are dissociated
elsewhere on the sun's surface. These lines and shadings are shown in
Fig. 211.

[Illustration: Fig. 211.]

It often happens that certain of the spectral lines are reversed in the
spectrum of the spot, a thin bright line appearing over the centre of a
thick dark one, as shown in Fig. 212. These reversals are due to very
bright vapors floating over the spot.

[Illustration: Fig. 212.]

At times, also, the spectrum of a spot indicates violent motion in the
overlying gases by distortion and displacement of the lines. This
phenomenon occurs oftener at points near the outer edge of the penumbra
than over the centre of the spot; but occasionally the whole
neighborhood is violently agitated. In such cases, lines in the spectrum
side by side are often affected in entirely different ways, one being
greatly displaced while its neighbor is not disturbed in the least,
showing that the vapors which produce the lines are at different levels
in the solar atmosphere, and moving independently of each other.

[Illustration: Fig. 213.]

192. _The Cause and Nature of Sun-Spots._--According to Professor Young,
the arrangement and relations of the photospheric clouds in the
neighborhood of a spot are such as are represented in Fig. 213. "Over
the sun's surface generally, these clouds probably have the form of
vertical columns, as at _aa_. Just outside the spot, the level of the
photosphere is the most part, overtopped by eruptions of hydrogen and
usually raised into faculæ, as at _bb_. These faculæ are, for metallic
vapors, as indicated by the shaded clouds.... While the great clouds of
hydrogen are found everywhere upon the sun, these spiky, vivid outbursts
of metallic vapors seldom occur except just in the neighborhood of a
spot, and then only during its season of rapid change. In the penumbra
of the spot the photospheric filaments become more or less nearly
horizontal, as at _pp_; in the umbra at _u_ it is quite uncertain what
the true state of affairs may be. We have conjecturally represented the
filaments there as vertical also, but depressed and carried down by a
descending current. Of course, the cavity is filled by the gases which
overlie the photosphere; and it is easy to see, that, looked at from
above, such a cavity and arrangement of the luminous filaments would
present the appearances actually observed."

Professor Young also suggests that the spots may be depressions in the
photosphere caused "by the _diminution of upward pressure_ from below,
in consequence of eruptions in the neighborhood; the spots thus being,
so to speak, _sinks_ in the photosphere. Undoubtedly the photosphere is
not a strictly continuous shell or crust; but it is _heavy_ as compared
with the uncondensed vapors in which it lies, just as a rain-cloud in
our terrestrial atmosphere is heavier than the air; and it is probably
continuous enough to have its upper level affected by any diminution of
pressure below. The gaseous mass below the photosphere supports its
weight and the weight of the products of condensation, which must always
be descending in an inconceivable rain and snow of molten and
crystallized material. To all intents and purposes, though nothing but a
layer of clouds, the photosphere thus forms a constricting shell, and
the gases beneath are imprisoned and compressed. Moreover, at a high
temperature the viscosity of gases is vastly increased, so that quite
probably the matter of the solar nucleus resembles pitch or tar in its
consistency more than what we usually think of as a gas. Consequently,
any sudden diminution of pressure would propagate itself slowly from the
point where it occurred. Putting these things together, it would seem,
that, whenever a free outlet is obtained through the photosphere at any
point, thus decreasing the inward pressure, the result would be the
sinking of a portion of the photosphere somewhere in the immediate
neighborhood, to restore the equilibrium; and, if the eruption were kept
up for any length of time, the depression in the photosphere would
continue till the eruption ceased. This depression, filled with the
overlying gases, would constitute a spot. Moreover, the line of fracture
(if we may call it so) at the edges of the sink would be a region of
weakness in the photosphere, so that we should expect a series of
eruptions all around the spot. For a time the disturbance, therefore,
would grow, and the spot would enlarge and deepen, until, in spite of
the viscosity of the internal gases, the equilibrium of pressure was
gradually restored beneath. So far as we know the spectroscopic and
visual phenomena, none of them contradict this hypothesis. There is
nothing in it, however, to account for the distribution of the spots in
solar latitudes, nor for their periodicity."


                 IV. THE CHROMOSPHERE AND PROMINENCES.


193. _The Sun's Outer Atmosphere._--What we see of the sun under
ordinary circumstances is but a fraction of his total bulk. While by far
the greater portion of the solar _mass_ is included within the
photosphere, the larger portion of his _volume_ lies without, and
constitutes a gaseous envelope whose diameter is at least double, and
its bulk therefore sevenfold, that of the central globe.

This outer envelope, though mainly gaseous, is not spherical, but has an
exceedingly irregular and variable outline. It seems to be made up, not
of regular strata of different density, like our atmosphere, but rather
of flames, beams, and streamers, as transient and unstable as those of
the aurora borealis. It is divided into two portions by a boundary as
definite, though not so regular, as that which separates them both from
the photosphere. The outer and far more extensive portion, which in
texture and rarity seems to resemble the tails of comets, is known as
the _coronal atmosphere_, since to it is chiefly due the _corona_, or
glory, which surrounds the darkened sun during an eclipse.

194. _The Chromosphere._--At the base of the coronal atmosphere, and in
contact with the photosphere, is what resembles a sheet of scarlet fire.
It appears as if countless jets of heated gas were issuing through vents
over the whole surface, clothing it with flame, which heaves and tosses
like the blaze of a conflagration. This is the _chromosphere_, or
color-sphere. It owes its vivid redness to the predominance of hydrogen
in the flames. The average depth of the chromosphere is not far from ten
or twelve seconds, or five thousand or six thousand miles.

195. _The Prominences._--Here and there masses of this hydrogen, mixed
with other substances, rise far above the general level into the coronal
regions, where they float like clouds, or are torn to pieces by
conflicting currents. These cloud-masses are known as solar
_prominences_, or _protuberances_.

196. _Magnitude and Distribution of the Prominences._--The prominences
differ greatly in magnitude. Of the 2,767 observed by Secchi, 1,964
attained an altitude of eighteen thousand miles; 751, or nearly a fourth
of the whole, reached a height of twenty-eight thousand miles; several
exceeded eighty-four thousand miles. In rare instances they reach
elevations as great as a hundred thousand miles. A few have been seen
which exceeded a hundred and fifty thousand miles; and Secchi has
recorded one of three hundred thousand miles.

[Illustration: Fig. 214.]

The irregular lines on the right-hand side of Fig. 214 show the
proportion of the prominences observed by Secchi, that were seen in
different parts of the sun's surface. The outer line shows the
distribution of the smaller prominences, and the inner dotted line that
of the larger prominences. By comparing these lines with those on the
opposite side of the circle, which show the distribution of the spots,
it will be seen, that, while the spots are confined mainly to two belts,
the prominences are seen in all latitudes.

197. _The Spectrum of the Chromosphere._--The spectrum of the
chromosphere is comparatively simple. There are eleven lines only which
are always present; and six of these are lines of hydrogen, and the
others, with a single exception, are of unknown elements. There are
sixteen other lines which make their appearance very frequently. Among
these latter are lines of sodium, magnesium, and iron.

Where some special disturbance is going on, the spectrum at the base of
the chromosphere is very complicated, consisting of hundreds of bright
lines. "The majority of the lines, however, are seen only occasionally,
for a few minutes at a time, when the gases and vapors, which generally
lie low (mainly in the interstices of the clouds which constitute the
photosphere), and below its upper surface, are elevated for the time
being by some eruptive action. For the most part, the lines which appear
only at such times are simply _reversals_ of the more prominent dark
lines of the ordinary solar spectrum. But the selection of the lines
seems most capricious: one is taken, and another left, though belonging
to the same element, of equal intensity, and close beside the first."
Some of the main lines of the chromosphere and prominences are shown in
Fig. 215.

[Illustration: Fig. 215.]

198. _Method of Studying the Chromosphere and Prominences._--Until
recently, the solar atmosphere could be seen only during a total eclipse
of the sun; but now the spectroscope enables us to study the
chromosphere and the prominences with nearly the same facility as the
spots and faculæ.

The protuberances are ordinarily invisible, for the same reason that the
stars cannot be seen in the daytime; they are hidden by the intense
light reflected from our own atmosphere. If we could only get rid of
this aerial illumination, without at the same time weakening the light
of the prominences, the latter would become visible. This the
spectroscope enables us to accomplish. Since the air-light is reflected
sunshine, it of course presents the same spectrum as sunlight,--a
continuous band of color crossed by dark lines. Now, this sort of
spectrum is weakened by increase of dispersive power (159), because the
light is spread out into a longer ribbon, and made to cover a greater
area. On the other hand, the spectrum of the prominences, being composed
of bright lines, undergoes no such diminution by increased dispersion.

[Illustration: Fig. 216.]

When the spectroscope is used as a means of examining the prominences,
the slit is more or less widened. The telescope is directed so that the
image of that portion of the solar limb which is to be examined shall be
tangent to the opened slit, as in Fig. 216, which represents the
slit-plate of the spectroscope of its actual size, with the image of the
sun in the proper position for observation.

[Illustration: Fig. 217.]

If, now, a prominence exists at this part of the solar limb, and if the
spectroscope itself is so adjusted that the _C_ line falls in the centre
of the field of view, then one will see something like Fig. 217. "The
red portion of the spectrum will stretch athwart the field of view like
a scarlet ribbon with a darkish band across it; and in that band will
appear the prominences, like scarlet clouds, so like our own terrestrial
clouds, indeed, in form and texture, that the resemblance is quite
startling. One might almost think he was looking out through a
partly-opened door upon a sunset sky, except that there is no variety or
contrast of color; all the cloudlets are of the same pure scarlet hue.
Along the edge of the opening is seen the chromosphere, more brilliant
than the clouds which rise from it or float above it, and, for the most
part, made up of minute tongues and filaments."

199. _Quiescent Prominences._--The prominences differ as widely in form
and structure as in magnitude. The two principal classes are the
_quiescent_, _cloud-formed_, or _hydrogenous_, and the _eruptive_, or
_metallic_.

[Illustration: Plate 3.]

The _quiescent_ prominences resemble almost exactly our terrestrial
clouds, and differ among themselves in the same manner. They are often
of enormous dimensions, especially in horizontal extent, and are
comparatively permanent, often undergoing little change for hours and
days. Near the poles they sometimes remain during a whole solar
revolution of twenty-seven days. Sometimes they appear to lie upon the
limb of the sun, like a bank of clouds in the terrestrial horizon,
probably because they are so far from the edge that only their upper
portions are in sight. When fully seen, they are usually connected to
the chromosphere by slender columns, generally smallest at the base, and
often apparently made up of separate filaments closely intertwined, and
expanding upward. Sometimes the whole under surface is fringed with
pendent filaments. Sometimes they float entirely free from the
chromosphere; and in most cases the larger clouds are attended by
detached cloudlets. Various forms of quiescent prominences are shown in
Plate III. Other forms are given in Figs. 218 and 219.

[Illustration: Fig. 218.]

Their spectrum is usually very simple, consisting of the four lines of
hydrogen and the orange _D_^3: hence the appellation _hydrogenous_.
Occasionally the sodium and magnesium lines also appear, even near the
tops of the clouds.

[Illustration: Fig. 219.]

200. _Eruptive Prominences._--The _eruptive_ prominences ordinarily
consist of brilliant spikes or jets, which change very rapidly in form
and brightness. As a rule, their altitude is not more than twenty
thousand or thirty thousand miles; but occasionally they rise far higher
than even the largest of the quiescent protuberances. Their spectrum is
very complicated, especially near their base, and often filled with
bright lines. The most conspicuous lines are those of sodium, magnesium,
barium, iron, and titanium: hence Secchi calls them _metallic_
prominences.

[Illustration: Fig. 220.]

They usually appear in the immediate vicinity of a spot, never very near
the solar poles. They change with such rapidity, that the motion can
almost be seen with the eye. Sometimes, in the course of fifteen or
twenty minutes, a mass of these flames, fifty thousand miles high, will
undergo a total transformation; and in some instances their complete
development or disappearance takes no longer time. Sometimes they
consist of pointed rays, diverging in all directions, as represented in
Fig. 220. "Sometimes they look like flames, sometimes like sheaves of
grain, sometimes like whirling water-spouts capped with a great cloud;
occasionally they present most exactly the appearance of jets of liquid
fire, rising and falling in graceful parabolas; frequently they carry on
their edges spirals like the volutes of an Ionic column; and continually
they detach filaments, which rise to a great elevation, gradually
expanding and growing fainter as they ascend, until the eye loses them."

[Illustration: Fig. 221.]

201. _Change of Form in Prominences._--Fig. 221 represents a prominence
as seen by Professor Young, Sept. 7, 1871. It was an immense quiescent
cloud, a hundred thousand miles long and fifty-four thousand miles high.
At _a_ there was a brilliant lump, somewhat in the form of a
thunder-head. On returning to the spectroscope less than half an hour
afterwards, he found that the cloud had been literally blown into shreds
by some inconceivable uprush from beneath. The prominence then presented
the form shown in Fig. 222. The _débris_ of the cloud had already
attained a height of a hundred thousand miles. While he was watching
them for the next ten minutes, they rose, with a motion almost
perceptible to the eye, till the uppermost reached an altitude of two
hundred thousand miles. As the filaments rose, they gradually faded away
like a dissolving cloud.

[Illustration: Fig. 222.]

Meanwhile the little thunder-head had grown and developed into what
appeared to be a mass of rolling and ever-changing flame. Figs. 223 and
224 give the appearance of this portion of the prominence at intervals
of fifteen minutes. Other similar eruptions have been observed.

[Illustration: Fig. 223.]

[Illustration: Fig. 224.]


                             V. THE CORONA.


202. _General Appearance of the Corona._--At the time of a total eclipse
of the sun, if the sky is clear, the moon appears as a huge black ball,
the illumination at the edge of the disk being just sufficient to bring
out its rotundity. "From behind it," to borrow Professor Young's vivid
description, "stream out on all sides radiant filaments, beams, and
sheets of pearly light, which reach to a distance sometimes of several
degrees from the solar surface, forming an irregular stellate halo, with
the black globe of the moon in its apparent centre. The portion nearest
the sun is of dazzling brightness, but still less brilliant than the
prominences which blaze through it like carbuncles. Generally this inner
corona has a pretty uniform height, forming a ring three or four minutes
of arc in width, separated by a somewhat definite outline from the outer
corona, which reaches to a much greater distance, and is far more
irregular in form. Usually there are several _rifts_, as they have been
called, like narrow beams of darkness, extending from the very edge of
the sun to the outer night, and much resembling the cloud-shadows which
radiate from the sun before a thunder-shower; but the edges of these
rifts are frequently curved, showing them to be something else than real
shadows. Sometimes there are narrow bright streamers, as long as the
rifts, or longer. These are often inclined, occasionally are even nearly
tangential to the solar surface, and frequently are curved. On the
whole, the corona is usually less extensive and brilliant over the solar
poles, and there is a recognizable tendency to accumulations above the
middle latitudes, or spot-zones; so that, speaking roughly, the corona
shows a disposition to assume the form of a quadrilateral or four-rayed
star, though in almost every individual case this form is greatly
modified by abnormal streamers at some point or other."

[Illustration: Fig. 225.]

203. _The Corona as seen at Recent Eclipses._--The corona can be seen
only at the time of a total eclipse of the sun, and then for only a few
minutes. Its form varies considerably from one eclipse to another, and
apparently also during the same eclipse. At least, different observers
at different stations depict the same corona under very different forms.
Fig. 225 represents the corona of 1857 as observed by Liais. In this
view the _petal-like_ forms, which have been noticed in the corona at
other times, are especially prominent.

[Illustration: Fig. 226.]

Fig. 226 shows the corona of 1860 as it was observed by Temple.

[Illustration: Fig. 227.]

Fig. 227 shows the corona of 1867. This is interesting as being a corona
at the time of sun-spot minimum.

[Illustration: Fig. 228.]

Fig. 228 represents the corona of 1868. This is a larger and more
irregular corona than usual.

[Illustration: Fig. 229.]

The corona of 1869 is shown in Fig. 229.

[Illustration: Fig. 230.]

Fig. 230 is a view of the corona of 1871 as seen by Capt. Tupman.

[Illustration: Fig. 231.]

Fig. 231 shows the same corona as seen by Foenander.

[Illustration: Fig. 232.]

Fig. 232 shows the same corona as photographed by Davis.

[Illustration: Fig. 233.]

Fig. 233 shows the corona of 1878 made up from several views as combined
by Professor Young.

204. _The Spectrum of the Corona._--The chief line in the spectrum of
the corona is the one usually designated as 1474, and now known as the
_coronal_ line. It is seen as a dark line on the disk of the sun; and a
spectroscope of great dispersive power shows this dark line to be
closely double, the lower component being one of the iron lines, and the
upper the coronal line. This dark line is shown at _x_, Fig. 234.

[Illustration: Fig. 234.]

Besides this bright line, the hydrogen lines appear faintly in the
spectrum of the corona. The 1474 line has been sometimes traced with the
spectroscope to an elevation of nearly twenty minutes above the moon's
limb, and the hydrogen lines nearly as far; and the lines were just as
strong _in the middle of a dark rift_ as anywhere else.

The substance which produces the 1474 line is unknown as yet. It seems
to be something with a vapor-density far below that of hydrogen, which
is the lightest substance of which we have any knowledge. It can hardly
be an "allotropic" form of any terrestrial element, as some scientists
have suggested; for in the most violent disturbances in prominences and
near sun-spots, when the lines of hydrogen, magnesium, and other metals,
are contorted and shattered by the rush of the contending elements, this
line alone remains fine, sharp, and straight, a little brightened, but
not otherwise affected. For the present it remains, like a few other
lines in the spectrum, an unexplained mystery.

Besides bright lines, the corona shows also a faint continuous spectrum,
in which have been observed a few of the more prominent _dark_ lines of
the solar spectrum.

This shows, that, while the corona may be in the main composed of
glowing gas (as indicated by the bright lines of its spectrum), it also
contains considerable matter in such a state as to reflect the sunlight,
probably in the form of dust or fog.


                              V. ECLIPSES.


[Illustration: Fig. 235.]

205. _The Shadows of the Earth and Moon._--The shadows cast by the earth
and moon are shown in Fig. 235. Each shadow is seen to be made up of a
dark portion called the _umbra_, and of a lighter portion called the
_penumbra_. The light of the sun is completely excluded from the umbra,
but only partially from the penumbra. The umbra is in the form of a
cone, with its apex away from the sun; though in the case of the earth's
shadow it tapers very slowly. The penumbra surrounds the umbra, and
increases in size as we recede from the sun. The axis of the earth's
shadow lies in the plane of the ecliptic, which in the figure is the
surface of the page. As the moon's orbit is inclined five degrees to the
plane of the ecliptic, the axis of the moon's shadow will sometimes lie
above, and sometimes below, the ecliptic. It will lie on the ecliptic
only when the moon is at one of her nodes.

206. _When there will be an Eclipse of the Moon._--The moon is eclipsed
_whenever it passes into the umbra of the earth's shadow_. It will be
seen from the figure that the moon can pass into the shadow of the earth
only when she is in opposition, or _at full_. Owing to the inclination
of the moon's orbit to the ecliptic, the moon will pass either above or
below the earth's shadow when she is at full, unless she happens to be
near her node at this time: hence there is not an eclipse of the moon
every month.

When the moon simply passes into the penumbra of the earth's shadow, the
light of the moon is somewhat dimmed, but not sufficiently to attract
attention, or to be denominated an eclipse.

[Illustration: Fig. 236.]

207. _The Lunar Ecliptic Limits._--In Fig. 236 the line _AB_ represents
the plane of the ecliptic, and the line _CD_ the moon's orbit. The large
black circles on the line _AB_ represent sections of the umbra of the
earth's shadow, and the smaller circles on _CD_ represent the moon at
full. It will be seen, that, if the moon is full at _E_, she will just
graze the umbra of the earth's shadow. In this case she will suffer no
eclipse. Were the moon full at any point nearer her node, as at _F_, she
would pass into the umbra of the earth's shadow, and would be
_partially_ eclipsed. Were the moon full at _G_, she would pass through
the centre of the earth's shadow, and be _totally_ eclipsed.

It will be seen from the figure that full moon must occur when the moon
is within a certain distance from her node, in order that there may be a
lunar eclipse; and this space is called the _lunar ecliptic limits_.

The farther the earth is from the sun, the less rapidly does its shadow
taper, and therefore the greater its diameter at the distance of the
moon; and, the nearer the moon to the earth, the greater the diameter of
the earth's shadow at the distance of the moon. Of course, the greater
the diameter of the earth's shadow, the greater the ecliptic limits:
hence the lunar ecliptic limits vary somewhat from time to time,
according to the distance from the earth to the sun and from the earth
to the moon. The limits within which an eclipse is inevitable under all
circumstances are called the _minor ecliptic limits_; and those within
which an eclipse is possible under some circumstances, the _major
ecliptic limits_.

[Illustration: Fig. 237.]

208. _Lunar Eclipses._--Fig. 237 shows the path of the moon through the
earth's shadow in the case of a _partial eclipse_. The magnitude of such
an eclipse depends upon the nearness of the moon to her nodes. The
magnitude of an eclipse is usually denoted in _digits_, a digit being
one-twelfth of the diameter of the moon.

[Illustration: Fig. 238.]

Fig. 238 shows the path of the moon through the earth's shadow in the
case of a _total eclipse_. It will be seen from the figure that it is
not necessary for the moon to pass through the centre of the earth's
shadow in order to have a total eclipse. When the moon passes through
the centre of the earth's shadow, the eclipse is both _total_ and
_central_.

At the time of a total eclipse, the moon is not entirely invisible, but
shines with a faint copper-colored light. This light is refracted into
the shadow by the earth's atmosphere, and its amount varies with the
quantity of clouds and vapor in that portion of the atmosphere which the
sunlight must graze in order to reach the moon.

The duration of an eclipse varies between very wide limits, being, of
course, greatest when the eclipse is central. A total eclipse of the
moon may last nearly two hours, or, including the _partial_ portions of
the eclipse, three or four hours.

Every eclipse of the moon, whether total or partial, is visible at the
same time to the whole hemisphere of the earth which is turned towards
the moon; and the eclipse will have exactly the same magnitude at every
point of observation.

209. _When there will be an Eclipse of the Sun._--There will be an
eclipse of the sun _whenever any portion of the moon's shadow is thrown
on the earth_. It will be seen from Fig. 235 that this can occur only
when the moon is in conjunction, or at _new_. It does not occur every
month, because, owing to the inclination of the moon's orbit to the
ecliptic, the moon's shadow is usually thrown either above or below the
earth at the time of new moon. There can be an eclipse of the sun only
when new moon occurs at or near one of the nodes of her orbit.

210. _Solar Ecliptic Limits._--The distances from the moon's node within
which a new moon would throw some portion of its shadow on the earth so
as to produce an eclipse of the sun are called the _solar ecliptic
limits_. As in the case of the moon, there are _major_ and _minor_
ecliptic limits; the former being the limits within which an eclipse of
the sun is _possible_ under some circumstances, and the latter those
under which an eclipse is _inevitable_ under all circumstances.

The limits within which a solar eclipse may occur are greater than those
within which a lunar eclipse may occur. This will be evident from an
examination of Fig. 235. Were the moon in that figure just outside of
the lines _AB_ and _CD_, it will be seen that the penumbra of her shadow
would just graze the earth: hence the moon must be somewhere within the
space bounded by these lines in order to cause an eclipse of the sun.
Now, these lines mark the prolongation to the sun of the cone of the
umbra of the earth's shadow: hence, in order to produce an eclipse of
the sun, new moon must occur somewhere within this prolongation of the
umbra of the earth's shadow. Now, it is evident that the diameter of
this cone is greater on the side of the earth toward the sun than on the
opposite side: hence the solar ecliptic limits are greater than the
lunar ecliptic limits.

211. _Solar Eclipses._--An observer in the umbra of the moon's shadow
would see a _total_ eclipse of the sun, while one in the penumbra would
see only a _partial_ eclipse. The magnitude of this partial eclipse
would depend upon the distance of the observer from the umbra of the
moon's shadow.

[Illustration: Fig. 239.]

[Illustration: Fig. 240.]

The umbra of the moon's shadow is just about long enough to reach the
earth. Sometimes the point of this shadow falls short of the earth's
surface, as shown in Fig. 239, and sometimes it falls upon the earth, as
shown in Fig. 240, according to the varying distance of the sun and moon
from the earth. The diameter of the umbra at the surface of the earth is
seldom more than a hundred miles: hence the belt of a total eclipse is,
on the average, not more than a hundred miles wide; and a total eclipse
seldom lasts more than five or six minutes, and sometimes only a few
seconds. Owing, however, to the rotation of the earth, the umbra of the
moon's shadow may pass over a long reach of the earth's surface. Fig.
241 shows the track of the umbra of the moon's shadow over the earth in
the total eclipse of 1860.

[Illustration: Fig. 241.]

[Illustration: Fig. 242.]

Fig. 242 shows the track of the total eclipse of 1871 across India and
the adjacent seas.

[Illustration: Fig. 243.]

[Illustration: Fig. 244.]

In a partial eclipse of the sun, more or less of one side of the sun's
disk is usually concealed, as shown in Fig. 243. Occasionally, however,
the centre of the sun's disk is covered, leaving a bright ring around
the margin, as shown in Fig. 244. Such an eclipse is called an _annular_
eclipse. An eclipse can be annular only when the cone of the moon's
shadow is too short to reach the earth, and then only to observers who
are in the central portion of the penumbra.

212. _Comparative Frequency of Solar and Lunar Eclipses._--There are
more eclipses of the sun in the year than of the moon; and yet, at any
one place, eclipses of the moon are more frequent than those of the sun.

There are more lunar than solar eclipses, because, as we have seen, the
limits within which a solar eclipse may occur are greater than those
within which a lunar eclipse may occur. There are more eclipses of the
moon visible at any one place than of the sun; because, as we have seen,
an eclipse of the moon, whenever it does occur, is visible to a whole
hemisphere at a time, while an eclipse of the sun is visible to only a
portion of a hemisphere, and a total eclipse to only a very small
portion of a hemisphere. A total eclipse of the sun is, therefore, a
very rare occurrence at any one place.

The greatest number of eclipses that can occur in a year is seven, and
the least number, two. In the former case, five may be of the sun and
two of the moon, or four of the sun and three of the moon. In the latter
case, both must be of the sun.


                    VI. THE THREE GROUPS OF PLANETS.


               I. GENERAL CHARACTERISTICS OF THE GROUPS.


213. _The Inner Group._--The _inner group_ of planets is composed of
_Mercury_, _Venus_, the _Earth_, and _Mars_; that is, of all the planets
which lie between the asteroids and the sun. The planets of this group
are comparatively small and dense. So far as known, they rotate on their
axes in about twenty-four hours, and they are either entirely without
moons, or are attended by comparatively few.

The comparative sizes and eccentricities of the orbits of this group are
shown in Fig. 245. The dots round the orbits show the position of the
planets at intervals of ten days.

[Illustration: Fig. 245.]

214. _The Outer Group._--The _outer group_ of planets is composed of
_Jupiter_, _Saturn_, _Uranus_, and _Neptune_. These planets are all very
large and of slight density. So far as known, they rotate on their axes
in about ten hours, and are accompanied with complicated systems of
moons. Fig. 246, which represents the comparative sizes of the planets,
shows at a glance the immense difference between those of the inner and
outer group. Fig. 247 shows the comparative sizes and eccentricities of
the orbits of the outer planets. The dots round the orbits show the
position of the planets at intervals of a thousand days.

[Illustration: Fig. 246.]

[Illustration: Fig. 247.]

215. _The Asteroids._--Between the inner and outer groups of planets
there is a great number of very small planets known as the _minor
planets_, or _asteroids_. Over two hundred planets belonging to this
group have already been discovered. Their orbits are shown by the dotted
lines in Fig. 247. The sizes of the four largest of these planets,
compared with the earth, are shown in Fig. 248.

[Illustration: Fig. 248.]

The asteroids of this group are distinguished from the other planets,
not only by their small size, but by the great eccentricities and
inclinations of their orbits. If we except Mercury, none of the larger
planets has an eccentricity amounting to one-tenth the diameter of its
orbit (43), nor is any orbit inclined more than two or three degrees to
the ecliptic; but the inclinations of many of the minor planets exceed
ten degrees, and the eccentricities frequently amount to an eighth of
the orbital diameter. The orbit of Pallas is inclined thirty-four
degrees to the ecliptic, while there are some planets of this group
whose orbits nearly coincide with the plane of the ecliptic.

[Illustration: Fig. 249.]

Fig. 249 shows one of the most and one of the least eccentric of the
orbits of this group as compared with that of the earth.

[Illustration: Fig. 250.]

The intricate complexity of the orbits of the asteroids is shown in Fig.
250.


                    II. THE INNER GROUP OF PLANETS.


                                Mercury.


216. _The Orbit of Mercury._--The orbit of Mercury is more eccentric
than that of any of the larger planets, and it has also a greater
inclination to the ecliptic. Its eccentricity (43) is a little over a
fifth, and its inclination to the ecliptic somewhat over seven degrees.
The mean distance of Mercury from the sun is about thirty-five million
miles; but, owing to the great eccentricity of its orbit, its distance
from the sun varies from about forty-three million miles at aphelion to
about twenty-eight million at perihelion.

[Illustration: Fig. 251.]

217. _Distance of Mercury from the Earth._--It is evident, from Fig.
251, that an inferior planet, like Mercury, is the whole diameter of its
orbit nearer the earth at inferior conjunction than at superior
conjunction: hence Mercury's distance from the earth varies
considerably. Owing to the great eccentricity of its orbit, its distance
from the earth at inferior conjunction also varies considerably. Mercury
is nearest to the earth when its inferior conjunction occurs at its own
aphelion and at the earth's perihelion.

[Illustration: Fig. 252.]

218. _Apparent Size of Mercury._--Since Mercury's distance from the
earth is variable, the apparent size of the planet is also variable.
Fig. 252 shows its apparent size at its extreme and mean distances from
the earth. Its apparent diameter varies from five seconds to twelve
seconds.

[Illustration: Fig. 253.]

219. _Volume and Density of Mercury._--The real diameter of Mercury is
about three thousand miles. Its size, compared with that of the earth,
is shown in Fig. 253. The earth is about sixteen times as large as
Mercury; but Mercury is about one-fifth more dense than the earth.

220. _Greatest Elongation of Mercury._--Mercury, being an _inferior_
planet (or one within the orbit of the earth), appears to oscillate to
and fro across the sun. Its greatest apparent distance from the sun, or
its _greatest elongation_, varies considerably. The farther Mercury is
from the sun, and the nearer the earth is to Mercury, the greater is its
angular distance from the sun at the time of its greatest elongation.
Under the most favorable circumstances, the greatest elongation amounts
to about twenty-eight degrees, and under the least favorable to only
sixteen or seventeen degrees.

221. _Sidereal and Synodical Periods of Mercury._--Mercury accomplishes
a complete revolution around the sun in about eighty-eight days; but it
takes it a hundred and sixteen days to pass from its greatest elongation
east to the same elongation again. The orbital motion of this planet is
at the rate of nearly thirty miles a second.

In Fig. 251, _P'''_ represents elongation east of the sun, and _P'_
elongation west. It will be seen that it is much farther from _P'_
around to _P'''_ than from _P'''_ on to _P'_. Mercury is only about
forty-eight days in passing from greatest elongation east to greatest
elongation west, while it is about sixty-eight days in passing back
again.

222. _Visibility of Mercury._--Mercury is too close to the sun for
favorable observation. It is never seen long after sunset, or long
before sunrise, and never far from the horizon. When visible at all, it
must be sought for low down in the west shortly after sunset, or low in
the east shortly before sunrise, according as the planet is at its east
or west elongation. It is often visible to the naked eye in our
latitude; but the illumination of the twilight sky, and the excess of
vapor in our atmosphere near the horizon, combine to make the telescopic
study of the planet difficult and unsatisfactory.

[Illustration: Fig. 254.]

223. _The Atmosphere and Surface of Mercury._--Mercury seems to be
surrounded by a dense atmosphere. One proof of the existence of such an
atmosphere is furnished at the time of the planet's _transit_ across the
disk of the sun, which occasionally happens. The planet is then seen
surrounded by a border, as shown in Fig. 254. A bright spot has also
been observed on the dark disk of the planet during a transit, as shown
in Fig. 255. The border around the planet seems to be due to the action
of the planet's atmosphere; but it is difficult to account for the
bright spot.

[Illustration: Fig. 255.]

[Illustration: Fig. 256.]

Schröter, a celebrated German astronomer, at about the beginning of the
present century, thought that he detected spots and shadings on the disk
of the planet, which indicated both the presence of an atmosphere and of
elevations. The shading along the terminator, which seemed to indicate
the presence of a twilight, and therefore of an atmosphere, are shown in
Fig. 256. It also shows the blunted aspect of one of the cusps, which
Schröter noticed at times, and which he attributed to the shadow of a
mountain, estimated to be ten or twelve miles high. Fig. 257 shows this
mountain near the upper cusp, as Schröter believed he saw it in the year
1800. By watching certain marks upon the disk of Mercury, Schröter came
to the conclusion that the planet rotates on its axis in about
twenty-four hours. Modern observers, with more powerful telescopes, have
failed to verify Schröter's observations as to the indications of an
atmosphere and of elevations. Nothing is known with certainty about the
rotation of the planet.

[Illustration: Fig. 257.]

The border around Mercury, and the bright spot on its disk at the time
of the transit of the planet across the sun, have been seen since
Schröter's time, and the existence of these phenomena is now well
established; but astronomers are far from being agreed as to their
cause.

224. _Intra-Mercurial Planets._--It has for some time been thought
probable that there is a group of small planets between Mercury and the
sun; and at various times the discovery of such bodies has been
announced. In 1859 a French observer believed that he had detected an
intra-Mercurial planet, to which the name of _Vulcan_ was given, and for
which careful search has since been made, but without success. During
the total eclipse of 1878 Professor Watson observed two objects near the
sun, which he thought to be planets; but this is still matter of
controversy.


                                 Venus.


225. _The Orbit of Venus._--The orbit of Venus has but slight
eccentricity, differing less from a circle than that of any other large
planet. It is inclined to the ecliptic somewhat more than three degrees.
The mean distance of the planet from the sun is about sixty-seven
million miles.

226. _Distance of Venus from the Earth._--The distance of Venus from the
earth varies within much wider limits than that of Mercury. When Venus
is at inferior conjunction, her distance from the earth is ninety-two
million miles _minus_ sixty-seven million miles, or twenty-five million
miles; and when at superior conjunction it is ninety-two million miles
_plus_ sixty-seven million miles, or a hundred and fifty-nine million
miles. Venus is considerably more than _six times_ as far off at
superior conjunction as at inferior conjunction.

[Illustration: Fig. 258.]

227. _Apparent Size of Venus._--Owing to the great variation in the
distance of Venus from the earth, her apparent diameter varies from
about ten seconds to about sixty-six seconds. Fig. 258 shows the
apparent size of Venus at her extreme and mean distances from the earth.

228. _Volume and Density of Venus._--The real size of Venus is about the
same as that of the earth, her diameter being only about three hundred
miles less. The comparative sizes of the two planets are shown in Fig.
259. The density of Venus is a little less than that of the earth.

[Illustration: Fig. 259.]

229. _The Greatest Elongation of Venus._--Venus, like Mercury, appears
to oscillate to and fro across the sun. The angular value of the
greatest elongation of Venus varies but slightly, its greatest value
being about forty-seven degrees.

230. _Sidereal and Synodical Periods of Venus._--The _sidereal_ period
of Venus, or that of a complete revolution around the sun, is about two
hundred and twenty-five days; her orbital motion being at the rate of
nearly twenty-two miles a second. Her _synodical_ period, or the time it
takes her to pass around from her greatest eastern elongation to the
same elongation again, is about five hundred and eighty-four days, or
eighteen months. Venus is a hundred and forty-six days, or nearly five
months, in passing from her greatest elongation east through inferior
conjunction to her greatest elongation west.

231. _Venus as a Morning and an Evening Star._--For a period of about
nine months, while Venus is passing from superior conjunction to her
greatest eastern elongation, she will be east of the sun, and will
therefore set after the sun. During this period she is the _evening
star_, the _Hesperus_ of the ancients. While passing from inferior
conjunction to superior conjunction, Venus is west of the sun, and
therefore rises before the sun. During this period of nine months she is
the _morning star_, the _Phosphorus_, or _Lucifer_, of the ancients.

232. _Brilliancy of Venus._--Next to the sun and moon, Venus is at times
the most brilliant object in the heavens, being bright enough to be seen
in daylight, and to cast a distinct shadow at night. Her brightness,
however, varies considerably, owing to her phases and to her varying
distance from the earth. She does not appear brightest when at full, for
she is then farthest from the earth, at superior conjunction; nor does
she appear brightest when nearest the earth, at inferior conjunction,
for her phase is then a thin crescent (see Fig. 258). She is most
conspicuous while passing from her greatest eastern elongation to her
greatest western elongation. After she has passed her eastern
elongation, she becomes brighter and brighter till she is within about
forty degrees of the sun. Her phase at this point in her orbit is shown
in Fig. 260. Her brilliancy then begins to wane, until she comes too
near the sun to be visible. When she re-appears on the west of the sun,
she again becomes more brilliant; and her brilliancy increases till she
is about forty degrees from the sun, when she is again at her brightest.
Venus passes from her greatest brilliancy as an evening star to her
greatest brilliancy as a morning star in about seventy-three days. She
has the same phase, and is at the same distance from the earth, in both
cases of maximum brilliancy. Of course, the brilliancy of Venus when at
the maximum varies somewhat from time to time, owing to the
eccentricities of the orbits of the earth and of Venus, which cause her
distance from the earth, at her phase of greatest brilliancy, to vary.
She is most brilliant when the phase of her greatest brilliancy occurs
when she is at her aphelion and the earth at its perihelion.

[Illustration: Fig. 260.]

233. _The Atmosphere and Surface of Venus._--Schröter believed that he
saw shadings and markings on Venus similar to those on Mercury,
indicating the presence of an atmosphere and of elevations on the
surface of the planet. Fig. 261 represents the surface of Venus as it
appeared to this astronomer. By watching certain markings on the disk of
Venus, Schröter came to the conclusion that Venus rotates on her axis in
about twenty-four hours.

[Illustration: Fig. 261.]

It is now generally conceded that Venus has a dense atmosphere; but
Schröter's observations of the spots on her disk have not been verified
by modern astronomers, and we really know nothing certainly of her
rotation.

234. _Transits of Venus._--When Venus happens to be near one of the
nodes of her orbit when she is in inferior conjunction, she makes a
transit across the sun's disk. These transits occur in pairs, separated
by an interval of over a hundred years. The two transits of each pair
are separated by an interval of eight years, the dates of the most
recent being 1874 and 1882. Venus, like Mercury, appears surrounded with
a border on passing across the sun's disk, as shown in Fig. 262.

[Illustration: Fig. 262.]


                                 Mars.


235. _The Orbit of Mars._--The orbit of Mars is more eccentric than that
of any of the larger planets, except Mercury; its eccentricity being
about one-eleventh. The inclination of the orbit to the ecliptic is
somewhat under two degrees. The mean distance of Mars from the sun is
about a hundred and forty million miles; but, owing to the eccentricity
of his orbit, the distance varies from a hundred and fifty-three million
miles to a hundred and twenty-seven million miles.

[Illustration: Fig. 263.]

236. _Distance of Mars from the Earth._--It will be seen, from Fig. 263,
that a _superior_ planet (or one outside the orbit of the earth), like
Mars, is nearer the earth, by the whole diameter of the earth's orbit,
when in opposition than when in conjunction. The mean distance of Mars
from the earth, at the time of opposition, is a hundred and forty
million miles _minus_ ninety-two million miles, or forty-eight million
miles. Owing to the eccentricity of the orbit of the earth and of Mars,
the distance of this planet when in opposition varies considerably. When
the earth is in aphelion, and Mars in perihelion, at the time of
opposition, the distance of the planet from the earth is only about
thirty-three million miles. On the other hand, when the earth is in
perihelion, and Mars in aphelion, at the time of opposition, the
distance of the planet is over sixty-two million miles.

The mean distance of Mars from the earth when in conjunction is a
hundred and forty million miles _plus_ ninety-two million miles, or two
hundred and thirty-two million miles. It will therefore be seen that
Mars is nearly five times as far off at conjunction as at opposition.

[Illustration: Fig. 264.]

237. _The Apparent Size of Mars._--Owing to the varying distance of Mars
from the earth, the apparent size of the planet varies almost as much as
that of Venus. Fig. 264 shows the apparent size of Mars at its extreme
and mean distances from the earth. The apparent diameter varies from
about four seconds to about thirty seconds.

[Illustration: Fig. 265.]

238. _The Volume and Density of Mars._--Among the larger planets Mars is
next in size to Mercury. Its real diameter is somewhat more than four
thousand miles, and its bulk is about one-seventh of that of the earth.
Its size, compared with that of the earth, is shown in Fig. 265.

[Illustration: Plate 4.]

The density of Mars is only about three-fourths of that of the earth.

239. _Sidereal and Synodical Periods of Mars._--The _sidereal_ period of
Mars, or the time in which he makes a complete revolution around the
sun, is about six hundred and eighty-seven days, or nearly twenty-three
months; but he is about seven hundred and eighty days in passing from
opposition to opposition again, or in performing a _synodical_
revolution. Mars moves in his orbit at the rate of about fifteen miles a
second.

240. _Brilliancy of Mars._--When near his opposition, Mars is easily
recognized with the naked eye by his fiery-red light. He is much more
brilliant at some oppositions than at others, for reasons already
explained (236), but always shines brighter than an ordinary star of the
first magnitude.

241. _Telescopic Appearance of Mars._--When viewed with a good telescope
(see Plate IV.), Mars is seen to be covered with dusky, dull-red
patches, which are supposed to be continents, like those of our own
globe. Other portions, of a greenish hue, are believed to be tracts of
water. The ruddy color, which overpowers the green, and makes the whole
planet seem red to the naked eye, was believed by Sir J. Herschel to be
due to an ochrey tinge in the general soil, like that of the red
sandstone districts on the earth. In a telescope, Mars appears less red,
and the higher the power the less the intensity of the color. The disk,
when well seen, is mapped out in a way which gives at once the
impression of land and water. The bright part is red inclining to
orange, sometimes dotted with brown and greenish points. The darker
spaces, which vary greatly in depth of tone, are of a dull gray-green,
having the aspect of a fluid which absorbs the solar rays. The
proportion of land to water on the earth appears to be reversed on Mars.
On the earth every continent is an island; on Mars all seas are lakes.
Long, narrow straits are more common than on the earth; and wide
expanses of water, like our Atlantic Ocean, are rare. (See Fig. 266.)

[Illustration: Fig. 266.]

[Illustration: Fig. 267.]

Fig. 267 represents a chart of the surface of Mars, which has been
constructed from careful telescopic observation. The outlines, as seen
in the telescope, are, however, much less distinct than they are
represented here; and it is by no means certain that the light and dark
portions are bodies of land and water.

In the vicinity of the poles brilliant white spots may be noticed, which
are considered by many astronomers to be masses of snow. This conjecture
is favored by the fact that they appear to diminish under the sun's
influence at the beginning of the Martial summer, and to increase again
on the approach of winter.

242. _Rotation of Mars._--On watching Mars with a telescope, the spots
on the disk are found to move (as shown in Fig. 268) in a manner which
indicates that the planet rotates in about twenty-four hours on an axis
inclined about twenty-eight degrees from a perpendicular to the plane of
its orbit. The inclination of the axis is shown in Fig. 269. It is
evident from the figure that the variation in the length of day and
night, and the change of seasons, are about the same on Mars as on the
earth. The changes will, of course, be somewhat greater, and the seasons
will be about twice as long.

[Illustration: Fig. 268.]

[Illustration: Fig. 269.]

[Illustration: Fig. 270.]

243. _The Satellites of Mars._--In 1877 Professor Hall of the Washington
Observatory discovered that Mars is accompanied by two small moons,
whose orbits are shown in Fig. 270. The inner satellite has been named
_Phobos_, and the outer one _Deimos_. It is estimated that the diameter
of the outer moon is from five to ten miles, and that of the inner one
from ten to forty miles.

Phobos is remarkable for its nearness to the planet and the rapidity of
its revolution, which is performed in seven hours thirty-eight minutes.
Its distance from the centre of the planet is about six thousand miles,
and from the surface less than four thousand. Astronomers on Mars, with
telescopes and eyes like ours, could readily find out whether this
satellite is inhabited, the distance being less than one-sixtieth of
that of our moon.

It will be seen that Phobos makes about three revolutions to one
rotation of the planet. It will, of course, rise in the west; though the
sun, the stars, and the other satellite rise in the east. Deimos makes a
complete revolution in about thirty hours.


                          III. THE ASTEROIDS.


244. _Bode's Law of Planetary Distances._--There is a very remarkable
law connecting the distances of the planets from the sun, which is
generally known by the name of _Bode's Law_. Attention was drawn to it
in 1778 by the astronomer Bode, but he was not really its author.

To express this law we write the following series of numbers:--

    0, 3, 6, 12, 24, 48, 96;

each number, with the exception of the first, being double the one which
precedes it. If we add 4 to each of these numbers, the series becomes--

    4, 7, 10, 16, 28, 52, 100;

which series was known to Kepler. These numbers, with the exception of
28, are sensibly proportional to the distances of the principal planets
from the sun, the actual distances being as follows:--

          Mercury. Venus.  Earth. Mars. ---- Jupiter. Saturn.

          3·9      7·2     10     15·2       52·9     95·4

245. _The First Discovery of the Asteroids._--The great gap between Mars
and Jupiter led astronomers, from the time of Kepler, to suspect the
existence of an unknown planet in this region; but no such planet was
discovered till the beginning of the present century. _Ceres_ was
discovered Jan. 1, 1801, _Pallas_ in 1802, _Juno_ in 1804, and _Vesta_
in 1807. Then followed a long interval of thirty-eight years before
_Astræa_, the fifth of these minor planets, was discovered in 1845.

246. _Olbers's Hypothesis._--After the discovery of Pallas, Olbers
suggested his celebrated hypothesis, that the two bodies might be
fragments of a single planet which had been shattered by some explosion.
If such were the case, the orbits of all the fragments would at first
intersect each other at the point where the explosion occurred. He
therefore thought it likely that other fragments would be found,
especially if a search were kept up near the intersection of the orbits
of Ceres and Pallas.

    Professor Newcomb makes the following observations concerning this
    hypothesis:--

    "The question whether these bodies could ever have formed a single
    one has now become one of cosmogony rather than of astronomy. If a
    planet were shattered, the orbit of each fragment would at first
    pass through the point at which the explosion occurred, however
    widely they might be separated through the rest of their course;
    but, owing to the secular changes produced by the attractions of the
    other planets, this coincidence would not continue. The orbits would
    slowly move away, and after the lapse of a few thousand years no
    trace of a common intersection would be seen. It is therefore
    curious that Olbers and his contemporaries should have expected to
    find such a region of intersection, as it implied that the explosion
    had occurred within a few thousand years. The fact that the required
    conditions were not fulfilled was no argument against the
    hypothesis, because the explosion might have occurred millions of
    years ago; and in the mean time the perihelion and node of each
    orbit would have made many entire revolutions, so that the orbits
    would have been completely mixed up.... A different explanation of
    the group is given by the nebular hypothesis; so that Olbers's
    hypothesis is no longer considered by astronomers."

247. _Later Discoveries of Asteroids._--Since 1845 over two hundred
asteroids have been discovered. All these are so small, that it requires
a very good telescope to see them; and even in very powerful telescopes
they appear as mere points of light, which can be distinguished from the
stars only by their motions.

To facilitate the discovery of these bodies, very accurate maps have
been constructed, including all the stars down to the thirteenth
magnitude in the neighborhood of the ecliptic. A reduced copy of one of
these maps is shown in Fig. 271.

[Illustration: Fig. 271.]

Furnished with a map of this kind, and with a telescope powerful enough
to show all the stars marked on it, the observer who is searching for
these small planets will place in the field of view of his telescope six
spider-lines at right angles to each other, and at equal distances
apart, in such a manner that several small squares will be formed,
embracing just as much of the heavens as do those shown in the map. He
will then direct his telescope to the region of the sky he wishes to
examine, represented by the map, so as to be able to compare
successively each square with the corresponding portion of the sky. Fig.
272 shows at the right hand the squares in the telescopic field of view,
and at the left hand the corresponding squares of the map.

[Illustration: Fig. 272.]

He can then assure himself if the numbers and positions of the stars
mapped, and of the stars observed, are identical. If he observes in the
field of view a luminous point which is not marked in the map, it is
evident that either the new body is a star of variable brightness which
was not visible at the time the map was made, or it is a planet, or
perhaps a comet. If the new body remains fixed at the same point, it is
the former; but, if it changes its position with regard to the
neighboring stars, it is the latter. The motion is generally so
sensible, that in the course of one evening the change of position may
be detected; and it can soon be determined, by the direction and rate of
the motion, whether the body is a planet or a comet.


                      IV. OUTER GROUP OF PLANETS.


                                Jupiter.


248. _Orbit of Jupiter._--The orbit of Jupiter is inclined only a little
over one degree to the ecliptic; and its eccentricity is only about half
of that of Mars, being less than one-twentieth. The mean distance of
Jupiter from the sun is about four hundred and eighty million miles;
but, owing to the eccentricity of his orbit, his actual distance from
the sun ranges from four hundred and fifty-seven to five hundred and
three million miles.

249. _Distance of Jupiter from the Earth._--When Jupiter is in
opposition, his mean distance from the earth is four hundred and eighty
million miles _minus_ ninety-two million miles, or three hundred and
eighty-eight million miles, and, when he is in conjunction, four hundred
and eighty million miles _plus_ ninety-two million miles, or five
hundred and seventy-two million miles. It will be seen that he is less
than twice as far off in conjunction as in opposition, and that the
ratio of his greatest to his least distance is very much less than in
the case of Venus and Mars. This is owing to his very much greater
distance from the sun. Owing to the eccentricities of the orbits of the
earth and of Jupiter, the greatest and least distances of Jupiter from
the earth vary somewhat from year to year.

[Illustration: Fig. 273.]

250. _The Brightness and Apparent Size of Jupiter._--The apparent
diameter of Jupiter varies from about fifty seconds to about thirty
seconds. His apparent size at his extreme and mean distances from the
earth is shown in Fig. 273.

Jupiter shines with a brilliant white light, which exceeds that of every
other planet except Venus. The planet is, of course, brightest when near
opposition.

251. _The Volume and Density of Jupiter._--Jupiter is the "giant planet"
of our system, his mass largely exceeding that of all the other planets
combined. His mean diameter is about eighty-five thousand miles; but the
equatorial exceeds the polar diameter by five thousand miles. In volume
he exceeds our earth about thirteen hundred times, but in mass only
about two hundred and thirteen times. His specific gravity is,
therefore, far less than that of the earth, and even less than that of
water. The comparative size of Jupiter and the earth is shown in Fig.
274.

[Illustration: Fig. 274.]

252. _The Sidereal and Synodical Periods of Jupiter._--It takes Jupiter
nearly twelve years to make a _sidereal_ revolution, or a complete
revolution around the sun, his orbital motion being at the rate of about
eight miles a second. His _synodical_ period, or the time of his passage
from opposition to opposition again, is three hundred and ninety-eight
days.

253. _The Telescopic Aspect of Jupiter._--There are no really permanent
markings on the disk of Jupiter; but his surface presents a very
diversified appearance. The earlier telescopic observers descried dark
belts across it, one north of the equator, and the other south of it.
With the increase of telescopic power, it was seen that these bands were
of a more complex structure than had been supposed, and consisted of
stratified, cloud-like appearances, varying greatly in form and number.
These change so rapidly, that the face of the planet rarely presents the
same appearance on two successive nights. They are most strongly marked
at some distance on each side of the planet's equator, and thus appear
as two belts under a low magnifying power.

Both the outlines of the belts, and the color of portions of the planet,
are subject to considerable changes. The equatorial regions, and the
spaces between the belts generally, are often of a rosy tinge. This
color is sometimes strongly marked, while at other times hardly a trace
of it can be seen. A general telescopic view of Jupiter is given in
Plate V.

[Illustration: Plate 5.]

254. _The Physical Constitution of Jupiter._--From the changeability of
the belts, and of nearly all the visible features of Jupiter, it is
clear that what we see on that planet is not the solid nucleus, but
cloud-like formations, which cover the entire surface to a great depth.
The planet appears to be covered with a deep and dense atmosphere,
filled with thick masses of clouds and vapor. Until recently this
cloud-laden atmosphere was supposed to be somewhat like that of our
globe; but at present the physical constitution of Jupiter is believed
to resemble that of the sun rather than that of the earth. Like the sun,
he is brighter in the centre than near the edges, as is shown in the
transits of the satellites over his disk. When the satellite first
enters on the disk, it commonly seems like a bright spot on a dark
background; but, as it approaches the centre, it appears like a dark
spot on the bright surface of the planet. The centre is probably two or
three times brighter than the edges. This may be, as in the case of the
sun, because the light near the edge passes through a greater depth of
atmosphere, and is diminished by absorption.

It has also been suspected that Jupiter shines partly by his own light,
and not wholly by reflected sunlight. The planet cannot, however, emit
any great amount of light; for, if it did, the satellites would shine by
this light when they are in the shadow of the planet, whereas they
totally disappear. It is possible that the brighter portions of the
surface are from time to time slightly self-luminous.

[Illustration: Fig. 275.]

Again: the interior of Jupiter seems to be the seat of an activity so
enormous that it can be ascribed only to intense heat. Rapid movements
are always occurring on his surface, often changing its aspect in a few
hours. It is therefore probable that Jupiter is not yet covered by a
solid crust, and that the fiery interior, whether liquid or gaseous, is
surrounded by the dense vapors which cease to be luminous on rising into
the higher and cooler regions of the atmosphere. Figs. 275 and 276 show
the disk of Jupiter as it appeared in December, 1881.

[Illustration: Fig. 276.]

255. _Rotation of Jupiter_.--Spots are sometimes visible which are much
more permanent than the ordinary markings on the belts. The most
remarkable of these is "the great red spot," which was first observed in
July, 1878, and is still to be seen in February, 1882. It is shown just
above the centre of the disk in Fig. 275. By watching these spots from
day to day, the time of Jupiter's axial rotation has been found to be
about nine hours and fifty minutes.

The axis of Jupiter deviates but slightly from a perpendicular to the
plane of its orbit, as is shown in Fig. 277.

[Illustration: Fig. 277.]


                       THE SATELLITES OF JUPITER.


[Illustration: Fig. 278.]

256. _Jupiter's Four Moons._--Jupiter is accompanied by four moons, as
shown in Fig. 278. The diameters of these moons range from about
twenty-two hundred to thirty-seven hundred miles. The second from the
planet is the smallest, and the third the largest. The smallest is about
the size of our moon; the largest considerably exceeds Mercury, and
almost rivals Mars, in bulk. The sizes of these moons, compared with
those of the earth and its moon, are shown in Fig. 279.

[Illustration: Fig. 279.]

The names of these satellites, in the order of their distance from the
planet, are _Io_, _Europa_, _Ganymede_, and _Callisto_. Their times of
revolution range from about a day and three-fourths up to about sixteen
days and a half. Their orbits are shown in Fig. 280.

[Illustration: Fig. 280.]

257. _The Variability of Jupiter's Satellites._--Remarkable variations
in the light of these moons have led to the supposition that violent
changes are taking place on their surfaces. It was formerly believed,
that, like our moon, they always present the same face to the planet,
and that the changes in their brilliancy are due to differences in the
luminosity of parts of their surface which are successively turned
towards us during a revolution; but careful measurements of their light
show that this hypothesis does not account for the changes, which are
sometimes very sudden. The satellites are too distant for examination of
their surfaces with the telescope: hence it is impossible to give any
certain explanation of these phenomena.

[Illustration: Fig. 281.]

258. _Eclipses of Jupiter's Satellites._--Jupiter, like the earth, casts
a shadow away from the sun, as shown in Fig. 281; and, whenever one of
his moons passes into this shadow, it becomes eclipsed. On the other
hand, whenever one of the moons throws its shadow on Jupiter, the sun is
eclipsed to that part of the planet which lies within the shadow.

To the inhabitants of Jupiter (if there are any, and if they can see
through the clouds) these eclipses must be very familiar affairs; for in
consequence of the small inclinations of the orbits of the satellites to
the planet's equator, and the small inclination of the latter to the
plane of Jupiter's orbit, all the satellites, except the most distant
one, are eclipsed in every revolution. A spectator on Jupiter might
therefore witness during the planetary year forty-five hundred eclipses
of the moons, and about the same number of the sun.

[Illustration: Fig. 282.]

259. _Transits of Jupiter's Satellites._--Whenever one of Jupiter's
moons passes in front of the planet, it is said to make a _transit_
across his disk. When a moon is making a transit, it presents its bright
hemisphere towards the earth, as will be seen from Fig. 282: hence it is
usually seen as a bright spot on the planet's disk; though sometimes, on
the brighter central portions of the disk, it appears dark.

[Illustration: Fig. 283.]

It will be seen from Fig. 282 that the shadow of a moon does not fall
upon the part of the planet's disk that is covered by the moon: hence we
may observe the transit of both the moon and its shadow. The shadow
appears as a small black spot, which will precede or follow the moon
according to the position of the earth in its orbit. Fig. 283 shows two
moons of Jupiter in transit.

260. _Occultations of Jupiter's Satellites._--The eclipse of a moon of
Jupiter must be carefully distinguished from the _occultation_ of a moon
by the planet. In the case of an eclipse, the moon ceases to be visible,
because the mass of Jupiter is interposed between the sun and the moon,
which ceases to be luminous, because the sun's light is cut off; but, in
the case of an occupation, the moon gets into such a position that the
body of Jupiter is interposed between it and the earth, thus rendering
the moon invisible to us. The third satellite, _m''_ (Fig. 282), is
invisible from the earth _E_, having become _occulted_ when it passed
behind the planet's disk; but it will not be _eclipsed_ until it passes
into the shadow of Jupiter.

261. _Jupiter without Satellites._--It occasionally happens that every
one of Jupiter's satellites will disappear at the same time, either by
being eclipsed or occulted, or by being in transit. In this event,
Jupiter will appear without satellites. This occurred on the 21st of
August, 1867. The position of Jupiter's satellites at this time is shown
in Fig. 284.

[Illustration: Fig. 284.]


                                Saturn.




                       THE PLANET AND HIS MOONS.


262. _The Orbit of Saturn._--The orbit of Saturn is rather more
eccentric than that of Jupiter, its eccentricity being somewhat more
than one-twentieth. Its inclination to the ecliptic is about two degrees
and a half. The mean distance of Saturn from the sun is about eight
hundred and eighty million miles. It is about a hundred million miles
nearer the sun at perihelion than at aphelion.

263. _Distance of Saturn from the Earth._--The mean distance of Saturn
from the earth at opposition is eight hundred and eighty million miles
_minus_ ninety-two million miles, or seven hundred and eighty-eight
million; and at conjunction, eight hundred and eighty million miles
_plus_ ninety-two million, or nine hundred and seventy-two million.
Owing to the eccentricity of the orbit of Saturn, his distance from the
earth at opposition and at conjunction varies by about a hundred million
miles at different times; but he is so immensely far away, that this is
only a small fraction of his mean distance.

264. _Apparent Size and Brightness of Saturn._--The apparent diameter of
Saturn varies from about twenty seconds to about fourteen seconds. His
apparent size at his extreme and mean distances from the earth is shown
in Fig. 285.

[Illustration: Fig. 285.]

The planet generally shines with the brilliancy of a moderate
first-magnitude star, and with a dingy, reddish light, as if seen
through a smoky atmosphere.

265. _Volume and Density of Saturn._--The real diameter of Saturn is
about seventy thousand miles, and its volume over seven hundred times
that of the earth. The comparative size of the earth and Saturn is shown
in Fig. 286. This planet is a little more than half as dense as Jupiter.

[Illustration: Fig. 286.]

266. _The Sidereal and Synodical Periods of Saturn._--Saturn makes a
complete revolution round the sun in a period of about twenty-nine years
and a half, moving in his orbit at the rate of about six miles a second.
The planet passes from opposition to opposition again in a period of
three hundred and seventy-eight days, or thirteen days over a year.

267. _Physical Constitution of Saturn._--The physical constitution of
Saturn seems to resemble that of Jupiter; but, being twice as far away,
the planet cannot be so well studied. The farther an object is from the
sun, the less it is illuminated; and, the farther it is from the earth,
the smaller it appears: hence there is a double difficulty in examining
the more distant planets. Under favorable circumstances, the surface of
Saturn is seen to be diversified with very faint markings; and, with
high telescopic powers, two or more very faint streaks, or belts, may be
discerned parallel to its equator. These belts, like those of Jupiter,
change their aspect from time to time; but they are so faint that the
changes cannot be easily followed. It is only on rare occasions that the
time of rotation can be determined from a study of the markings.

268. _Rotation of Saturn._--On the evening of Dec. 7, 1876, Professor
Hall, who had been observing the satellites of Saturn with the great
Washington telescope (18), saw a brilliant white spot near the equator
of the planet. It seemed as if an immense eruption of incandescent
matter had suddenly burst up from the interior. The spot gradually
spread itself out into a long light streak, of which the brightest point
was near the western end. It remained visible until January, when it
became faint and ill-defined, and the planet was lost in the rays of the
sun.

From all the observations on this spot, Professor Hall found the period
of Saturn to be ten hours fourteen minutes, reckoning by the brightest
part of the streak. Had the middle of the streak been taken, the time
would have been less, because the bright matter seemed to be carried
along in the direction of the planet's rotation. If this motion was due
to a wind, the velocity of the current must have been between fifty and
a hundred miles an hour. The axis of Saturn is inclined twenty-seven
degrees from the perpendicular to its orbit.

[Illustration: Fig. 287.]

269. _The Satellites of Saturn._--Saturn is accompanied by eight moons.
Seven of these are shown in Fig. 287. The names of these satellites, in
the order of their distances from the planet, are given in the
accompanying table:--

    Number. Name.      Distance   Sidereal              Discoverer.
                           from    Period.
                         Planet

          1 Mimas       120,800    0 22 37         0.94 Herschel

          2 Enceladus   155,000    1  8 53         1.37 Herschel

          3 Tethys      191,900    1 21 18         1.88 Cassini

          4 Dione       245,800    2 17 41         2.73 Cassini

          5 Rhea        343,400    4 12 25         4.51 Cassini

          6 Titan       796,100   15 22 41        15.94 Huyghens

          7 Hyperion    963,300   21  7  7        21.29 Bond

          8 Japetus   2,313,800   79  7 53        79.33 Cassini

The apparent brightness or visibility of these satellites follows the
order of their discovery. The smallest telescope will show Titan, and
one of very moderate size will show Japetus in the western part of its
orbit. An instrument of four or five inches aperture will show Rhea, and
perhaps Tethys and Dione; while seven or eight inches are required for
Enceladus, even at its greatest elongation from the planet. Mimas can
rarely be seen except at its greatest elongation, and then only with an
aperture of twelve inches or more. Hyperion can be detected only with
the most powerful telescopes, on account of its faintness and the
difficulty of distinguishing it from minute stars.

_Japetus_, the outermost satellite, is remarkable for the fact, that
while, in one part of its orbit, it is the brightest of the satellites
except Titan, in the opposite part it is almost as faint as Hyperion,
and can be seen only in large telescopes. When west of the planet, it is
bright; when east of it, faint. This peculiarity has been accounted for
by supposing that the satellite, like our moon, always presents the same
face to the planet, and that one side of it is white and the other
intensely black; but it is doubtful whether any known substance is so
black as one side of the satellite must be to account for such
extraordinary changes of brilliancy.

[Illustration: Fig. 288.]

_Titan_, the largest of these satellites, is about the size of the
largest satellite of Jupiter. The relative sizes of the satellites are
shown in Fig. 288, and their orbits in Fig. 289.

[Illustration: Fig. 289.]

[Illustration: Fig. 290.]

Fig. 290 shows the transit of one of the satellites, and of its shadow,
across the disk of the planet.


                          THE RINGS OF SATURN.


270. _General Appearance of the Rings._--Saturn is surrounded by a thin
flat ring lying in the plane of its equator. This ring is probably less
than a hundred miles thick. The part of it nearest Saturn reflects
little sunlight to us; so that it has a dusky appearance, and is not
easily seen, although it is not quite so dark as the sky seen between it
and the planet. The outer edge of this dusky portion of the ring is at a
distance from Saturn of between two and three times the earth's
diameter. Outside of this dusky part of the ring is a much brighter
portion, and outside of this another, which is somewhat fainter, but
still so much brighter than the dusky part as to be easily seen. The
width of the brighter parts of the ring is over three times the earth's
diameter. To distinguish the parts, the outer one is called ring _A_,
the middle one ring _B_, and the dusky one ring _C_. Between _A_ and _B_
is an apparently open space, nearly two thousand miles wide, which looks
like a black line on the ring. Other divisions in the ring have been
noticed at times; but this is the only one always seen with good
telescopes at times when either side of the ring is in view from the
earth. The general telescopic appearance of the ring is shown in Fig.
291.

[Illustration: Fig. 291.]

[Illustration: Fig. 292.]

Fig. 292 shows the divisions of the rings as they were seen by Bond.

271. _Phases of Saturn's Ring._--The ring is inclined to the plane of
the planet's orbit by an angle of twenty-seven degrees. The general
aspect from the earth is nearly the same as from the sun. As the planet
revolves around the sun, the axis and plane of the ring keep the same
direction in space, just as the axis of the earth and the plane of the
equator do.

When the planet is in one part of its orbit, we see the upper or
northern side of the ring at an inclination of twenty-seven degrees, the
greatest angle at which the ring can ever be seen. This phase of the
ring is shown in Fig. 293.

[Illustration: Fig. 293.]

When the planet has moved through a quarter of a revolution, the edge of
the ring is turned towards the sun and the earth; and, owing to its
extreme thinness, it is visible only in the most powerful telescopes as
a fine line of light, stretching out on each side of the planet. This
phase of the ring is shown in Fig. 294.

[Illustration: Fig. 294.]

All the satellites, except Japetus, revolve very nearly in the plane of
the ring: consequently, when the edge of the ring is turned towards the
earth, the satellites seem to swing from one side of the planet to the
other in a straight line, running along the thin edge of the ring like
beads on a string. This phase affords the best opportunity of seeing the
inner satellites, Mimas and Enceladus, which at other times are obscured
by the brilliancy of the ring.

[Illustration: Fig. 295.]

Fig. 295 shows a phase of the ring intermediate between the last two.

When the planet has moved ninety degrees farther, we again see the ring
at an angle of twenty-seven degrees; but now it is the lower or southern
side which is visible. When it has moved ninety degrees farther, the
edge of the ring is again turned towards the earth and sun.

[Illustration: Fig. 295.]

The successive phases of Saturn's ring during a complete revolution are
shown in Fig. 296.

It will be seen that there are two opposite points of Saturn's orbit in
which the rings are turned edgewise to us, and two points half-way
between the former in which the ring is seen at its maximum inclination
of about twenty-seven degrees. Since the planet performs a revolution in
twenty-nine years and a half, these phases occur at average intervals of
about seven years and four months.

[Illustration: Fig. 297.]

[Illustration: Fig. 298.]

272. _Disappearance of Saturn's Ring._--It will be seen from Fig. 297
that the plane of the ring may not be turned towards the sun and the
earth at exactly the same time, and also that the earth may sometimes
come on one side of the plane of the ring while the sun is shining on
the other. In the figure, _E_, _E'_, _E''_, and _E'''_ is the orbit of
the earth. When Saturn is at _S'_, or opposite, at _F_, the plane of the
ring will pass through the sun, and then only the edge of the ring will
be illumined. Were Saturn at _S_, and the earth at _E'_, the plane of
the ring would pass through the earth. This would also be the case were
the earth at _E'''_, and Saturn at _S''_. Were Saturn at _S_ or at
_S''_, and the earth farther to the left or to the right, the sun would
be shining on one side of the ring while we should be looking on the
other. In all these cases the ring will disappear entirely in a
telescope of ordinary power. With very powerful telescopes the ring will
appear, in the first two cases, as a thin line of light (Fig. 298). It
will be seen that all these cases of disappearance must take place when
Saturn is in the parts of his orbit intercepted between the parallel
lines _AC_ and _BD_. These lines are tangent to the earth's orbit, which
they enclose, and are parallel to the plane of Saturn's ring. As Saturn
passes away from these two lines on either side, the rings appear more
and more open. When the dark side of the ring is in view, it appears as
a black line crossing the planet; and on such occasions the sunlight
reflected from the outer and inner edges of the rings _A_ and _B_
enables us to see traces of the ring on each side of Saturn, at least in
places where two such reflections come nearly together. Fig. 299
illustrates this reflection from the edges at the divisions of the
rings.

[Illustration: Fig. 299.]

273. _Changes in Saturn's Ring._--The question whether changes are going
on in the rings of Saturn is still unsettled. Some observers have
believed that they saw additional divisions in the rings from time to
time; but these may have been errors of vision, due partly to the
shading which is known to exist on portions of the ring.

Professor Newcomb says, "As seen with the great Washington equatorial in
the autumn of 1874, there was no great or sudden contrast between the
inner or dark edge of the bright ring and the outer edge of the dusky
ring. There was some suspicion that the one shaded into the other by
insensible gradations. No one could for a moment suppose, as some
observers have, that there was a separation between these two rings. All
these considerations give rise to the question whether the dusky ring
may not be growing at the expense of the inner bright ring."

Struve, in 1851, advanced the startling theory that the inner edge of
the ring was gradually approaching the planet, the whole ring spreading
inwards, and making the central opening smaller. The theory was based
upon the descriptions and drawings of the rings by the astronomers of
the seventeenth century, especially Huyghens, and the measures made by
later astronomers up to 1851. This supposed change in the dimension of
the ring is shown in Fig. 300.

[Illustration: Fig. 300.]

274. _Constitution of Saturn's Ring._--The theory now generally held by
astronomers is, that the ring is composed of a cloud of satellites too
small to be separately seen in the telescope, and too close together to
admit of visible intervals between them. The ring looks solid, because
its parts are too small and too numerous to be seen singly. They are
like the minute drops of water that make up clouds and fogs, which to
our eyes seem like solid masses. In the dusky ring the particles may be
so scattered that we can see through the cloud, the duskiness being due
to the blending of light and darkness. Some believe, however, that the
duskiness is caused by the darker color of the particles rather than by
their being farther apart.


                                Uranus.


275. _Orbit and Dimensions of Uranus._--Uranus, the smallest of the
outer group of planets, has a diameter of nearly thirty-two thousand
miles. It is a little less dense than Jupiter, and its mean distance
from the sun is about seventeen hundred and seventy millions of miles.
Its orbit has about the same eccentricity as that of Jupiter, and is
inclined less than a degree to the ecliptic. Uranus makes a revolution
around the sun in eighty-four years, moving at the rate of a little over
four miles a second. It is visible to the naked eye as a star of the
sixth magnitude.

As seen in a large telescope, the planet has a decidedly sea-green
color; but no markings have with certainty been detected on its disk, so
that nothing is really known with regard to its rotation. Fig. 301 shows
the comparative size of Uranus and the earth.

[Illustration: Fig. 301.]

276. _Discovery of Uranus._--This planet was discovered by Sir William
Herschel in March, 1781. He was engaged at the time in examining the
small stars of the constellation _Gemini_, or the Twins. He noticed that
this object which had attracted his attention had an appreciable disk,
and therefore could not be a star. He also perceived by its motion that
it could not be a nebula; he therefore concluded that it was a comet,
and announced his discovery as such. On attempting to compute its orbit,
it was soon found that its motions could be accounted for only on the
supposition that it was moving in a circular orbit at about twice the
distance of Saturn from the sun. It was therefore recognized as a new
planet, whose discovery nearly doubled the dimensions of the solar
system as it was then known.

277. _The Name of the Planet._--Herschel, out of compliment to his
patron, George III., proposed to call the new planet _Georgium Sidus_
(the Georgian Star); but this name found little favor. The name of
_Herschel_ was proposed, and continued in use in England for a time, but
did not meet with general approval. Various other names were suggested,
and finally that of _Uranus_ was adopted.

[Illustration: Fig. 302.]

278. _The Satellites of Uranus._--Uranus is accompanied by four
satellites, whose orbits are shown in Fig. 302. These satellites are
remarkable for the great inclination of their orbits to the plane of the
planet's orbit, amounting to about eighty degrees, and for their
_retrograde_ motion; that is, they move _from east to west_, instead of
from west to east, as in the case of all the planets and of all the
satellites previously discovered.


                                Neptune.


279. _Orbit and Dimensions of Neptune._--So far as known, Neptune is the
most remote member of the solar system, its mean distance from the sun
being twenty-seven hundred and seventy-five million miles. This distance
is considerably less than twice that of Uranus. Neptune revolves around
the sun in a period of a little less than a hundred and sixty-five
years. Its orbit has but slight eccentricity, and is inclined less than
two degrees to the ecliptic. This planet is considerably larger than
Uranus, its diameter being nearly thirty-five thousand miles. It is
somewhat less dense than Uranus. Neptune is invisible to the naked eye,
and no telescope has revealed any markings on its disk: hence nothing is
certainly known as to its rotation. Fig. 303 shows the comparative size
of Neptune and the earth.

[Illustration: Fig. 303.]

280. _The Discovery of Neptune._--The discovery of Neptune was made in
1846, and is justly regarded as one of the grandest triumphs of
astronomy.

Soon after Uranus was discovered, certain irregularities in its motion
were observed, which could not be explained. It is well known that the
planets are all the while disturbing each other's motions, so that none
of them describe perfect ellipses. These mutual disturbances are called
_perturbations_. In the case of Uranus it was found, that, after making
due allowance for the action of all the known planets, there were still
certain perturbations in its course which had not been accounted for.
This led astronomers to the suspicion that these might be caused by an
unknown planet. Leverrier in France, and Adams in England, independently
of each other, set themselves the difficult problem of computing the
position and magnitude of a planet which would produce these
perturbations. Both, by a most laborious computation, showed that the
perturbations were such as would be produced by a planet revolving about
the sun at about twice the distance of Uranus, and having a mass
somewhat greater than that of this planet; and both pointed out the same
part of the heavens as that in which the planet ought to be found at
that time. Almost immediately after they had announced the conclusion to
which they had arrived, the planet was found with the telescope. The
astronomer who was searching for the planet at the suggestion of
Leverrier was the first to recognize it: hence Leverrier has obtained
the chief credit of the discovery.

The observed planet is proved to be nearer than the one predicted by
Leverrier and Adams, and therefore of smaller magnitude.

281. _The Observed Planet not the Predicted One._--Professor Peirce
always maintained that the planet found by observation was not the one
whose existence had been predicted by Leverrier and Adams, though its
action would completely explain all the irregularities in the motion of
Uranus. His last statement on this point is as follows: "My position is,
that there were _two possible planets_, either of which might have
caused the observed irregular motions of Uranus. Each planet excluded
the other; so that, if one was, the other was not. They coincided in
direction from the earth at certain epochs, once in six hundred and
fifty years. It was at one of these epochs that the prediction was made,
and at no other time for six centuries could the prediction of the one
planet have revealed the other. The observed planet was not the
predicted one."

282. _Bode's Law Disproved._--The following table gives the distances of
the planets according to Bode's law, their actual distances, and the
error of the law in each case:--

               Planet.      Numbers of     Actual Errors.
                                 Bode. Distances.


               Mercury     0 + 4 =   4        3.9     0.1

               Venus       3 + 4 =   7        7.2     0.2

               Earth       6 + 4 =  10       10.0     0.0

               Mars       12 + 4 =  16       15.2     0.8

               Minor      24 + 4 =  28   20 to 35
               planets

               Jupiter    48 + 4 =  52       52.0     0.0

               Saturn     96 + 4 = 100       95.4     4.6

               Uranus    192 + 4 = 196      191.9     4.1

               Neptune   384 + 4 = 388      300.6    87.4

It will be seen, that, before the discovery of Neptune, the agreement
was so close as to indicate that this was an actual law of the
distances; but the discovery of this planet completely disproved its
existence.

[Illustration: Fig. 304.]

283. _The Satellite of Neptune._--Neptune is accompanied by at least one
moon, whose orbit is shown in Fig. 304. The orbit of this satellite is
inclined about thirty degrees to the plane of the ecliptic, and the
motion of the satellite is retrograde, or from east to west.


                        VII. COMETS AND METEORS.


                               I. COMETS.


                      General Phenomena of Comets.

284. _General Appearance of a Bright Comet._--Comets bright enough to be
seen with the naked eye are composed of three parts, which run into each
other by insensible gradations. These are the _nucleus_, the _coma_, and
the _tail_.

The _nucleus_ is the bright centre of the comet, and appears to the eye
as a star or planet.

The _coma_ is a nebulous mass surrounding the nucleus on all sides.
Close to the nucleus it is almost as bright as the nucleus itself; but
it gradually shades off in every direction. The nucleus and coma
combined appear like a star shining through a small patch of fog; and
these two together form what is called the _head_ of the comet.

The _tail_ is a continuation of the coma, and consists of a stream of
milky light, growing wider and fainter as it recedes from the head, till
the eye is unable to trace it.

[Illustration: Fig. 305.]

The general appearance of one of the smaller of the brilliant comets is
shown in Fig. 305.

[Illustration: Fig. 306.]

[Illustration: Fig. 307.]

285. _General Appearance of a Telescopic Comet._--The great majority of
comets are too faint to be visible with the naked eye, and are called
_telescopic_ comets. In these comets there seems to be a development of
coma at the expense of nucleus and tail. In some cases the telescope
fails to reveal any nucleus at all in one of these comets; at other
times the nucleus is so faint and ill-defined as to be barely
distinguishable. Fig. 306 shows a telescopic comet without any nucleus
at all, and another with a slight condensation at the centre. In these
comets it is generally impossible to distinguish the coma from the tail,
the latter being either entirely invisible, as in Fig. 306, or else only
an elongation of the coma, as shown in Fig. 307. Many comets appear
simply as patches of foggy light of more or less irregular form.

[Illustration: Fig. 308.]

286. _The Development of Telescopic Comets on their Approach to the
Sun._--As a rule, all comets look nearly alike when they first come
within the reach of the telescope. They appear at first as little foggy
patches, without any tail, and often without any visible nucleus. As
they approach the sun their peculiarities are rapidly developed. Fig.
308 shows such a comet as first seen, and the gradual development of its
nucleus, head, and tail, as it approaches the sun.

[Illustration: Fig. 309.]

[Illustration: Fig. 310.]

[Illustration: Fig. 311.]

If the comet is only a small one, the tail developed is small; but these
small appendages have a great variety of form in different comets. Fig.
309 shows the singular form into which _Encke's_ comet was developed in
1871. Figs. 310 and 311 show other peculiar developments of telescopic
comets.

287. _Development of Brilliant Comets on their Approach to the
Sun._--Brilliant comets, as well as telescopic comets, appear nearly
alike when they come into the view of the telescope; and it is only on
their approach to the sun that their distinctive features are developed.
Not only do these comets, when they first come into view, resemble each
other, but they also bear a close resemblance to telescopic comets.

As the comet approaches the sun, bright vaporous jets, two or three in
number, are emitted from the nucleus on the side of the sun and in the
direction of the sun. These jets, though directed towards the sun, are
soon more or less carried backward, as if repelled by the sun. Fig. 312
shows a succession of views of these jets as they were developed in the
case of _Halley's_ comet in 1835.

[Illustration: Fig. 312.]

The jets in this case seemed to have an oscillatory motion. At 1 and 2
they seemed to be attracted towards the sun, and in 3 to be repelled by
him. In 4 and 5 they seemed to be again attracted, and in 6 to be
repelled, but in a reverse direction to that in 3. In 7 they appeared to
be again attracted. Bessel likened this oscillation of the jets to the
vibration of a magnetic needle when presented to the pole of a magnet.

In the case of larger comets these luminous jets are surrounded by one
or more envelops, which are thrown off in succession as the comet
approaches the sun. The formation of these envelops was a conspicuous
feature of _Donati's_ comet of 1858. A rough view of the jets and the
surrounding envelops is given in Fig. 313. Fig. 314 gives a view of the
envelops without the jets.

[Illustration: Fig. 313.]

[Illustration: Fig. 314.]

288. _The Tails of Comets._--The _tails_ of brilliant comets are rapidly
formed as the comet approaches the sun, their increase in length often
being at the rate of several million miles a day. These appendages seem
to be formed entirely out of the matter which is emitted from the
nucleus in the luminous jets which are at first directed towards the
sun. The tails of comets are, however, always directed away from the
sun, as shown in Fig. 315.

[Illustration: Fig. 315.]

It will be seen that the comet, as it approaches the sun, travels head
foremost; but as it leaves the sun it goes tail foremost.

The apparent length of the tail of a comet depends partly upon its real
length, partly upon the distance of the comet, and partly upon the
direction of the axis of the tail with reference to the line of vision.
The longer the tail, the nearer the comet; and the more nearly at right
angles to the line of vision is the axis of the tail, the greater is the
apparent length of the tail. In the majority of cases the tails of
comets measure only a few degrees; but, in the case of many comets
recorded in history, the tail has extended half way across the heavens.

The tail of a comet, when seen at all, is usually several million miles
in length; and in some instances the tail is long enough to reach across
the orbit of the earth, or twice as far as from the earth to the sun.

The tails of comets are apparently hollow, and are sometimes a million
of miles in diameter. So great, however, is the tenuity of the matter in
them, that the faintest stars are seen through it without any apparent
obscuration. See Fig. 316, which is a view of the great comet of 1264.

[Illustration: Fig. 316.]

[Illustration: Fig. 317.]

[Illustration: Fig. 318.]

[Illustration: Fig. 319.]

[Illustration: Fig. 320.]

The tails of comets are sometimes straight, as in Fig. 316, but usually
more or less curved, as in Fig. 317, which is a view of _Donati's_ comet
as it appeared at one time. The tail of a comet is occasionally divided
into a number of streamers, as in Figs. 318 and 319. Fig. 318 is a view
of the great comet of 1744, and Fig. 319 of the great comet of 1861. No.
1, in Fig. 320, is a view of the comet of 1577; No. 2, of the comet of
1680; and No. 3, of the comet of 1769.

[Illustration: Fig. 321.]

Fig. 321 shows some of the forms which the imagination of a
superstitious age saw depicted in comets, when these heavenly visitants
were thought to be the forerunners of wars, pestilence, famine, and
other dire calamities.

289. _Visibility of Comets._--Even the brightest comets are visible only
a short time near their perihelion passage. When near the sun, they
sometimes become very brilliant, and on rare occasions have been visible
even at mid-day. It is seldom that a comet can be seen, even with a
powerful telescope, during its perihelion passage, unless its perihelion
is either inside of the earth's orbit, or but little outside of it.


                      Motion and Origin of Comets.


290. _Recognition of a Telescopic Comet._--It is impossible to
distinguish telescopic comets by their appearance from another class of
heavenly bodies known as _nebulæ_. Such comets can be recognized only by
their motion. Thus, in Fig. 322, the upper and lower bodies look exactly
alike; but the upper one is found to remain stationary, while the lower
one moves across the field of view. The upper one is thus shown to be a
nebula, and the lower one a comet.

[Illustration: Fig. 322.]

291. _Orbits of Comets._--All comets are found to move in _very
eccentric ellipses_, in _parabolas_, or in _hyperbolas_.

Since an ellipse is a _closed_ curve (48), all comets that move in
ellipses, no matter how eccentric, are permanent members of the solar
system, and will return to the sun at intervals of greater or less
length, according to the size of the ellipses and the rate of the
comet's motion.

Parabolas and hyperbolas being _open_ curves (48), comets that move in
either of these orbits are only temporary members of our solar system.
After passing the sun, they move off into space, never to return, unless
deflected hither by the action of some heavenly body which they pass in
their journey.

[Illustration: Fig. 323.]

    Since a comet is visible only while it is near the sun, it is
    impossible to tell, by the form of the portion of the orbit which it
    describes during the period of its visibility, whether it is a part
    of a very elongated ellipse, a parabola, or a hyperbola. Thus in
    Fig. 323 are shown two orbits, one of which is a very elongated
    ellipse, and the other a parabola. The part _ab_, in each case, is
    the portion of the orbit described by the comet during its
    visibility. While describing the dotted portions of the orbit, the
    comet is invisible. Now it is impossible to distinguish the form of
    the visible portion in the two orbits. The same would be true were
    one of the orbits a hyperbola.

    Whether a comet will describe an ellipse, a parabola, or a
    hyperbola, can be determined only by its _velocity_, taken in
    connection with its _distance from the sun_. Were a comet ninety-two
    and a half million miles from the sun, moving away from the sun at
    the rate of twenty-six miles a second, it would have just the
    velocity necessary to describe a _parabola_. Were it moving with a
    greater velocity, it would necessarily describe a _hyperbola_, and,
    with a less velocity, an _ellipse_. So, at any distance from the
    sun, there is a certain velocity which would cause a comet to
    describe a parabola; while a greater velocity would cause it to
    describe a hyperbola, and a less velocity to describe an ellipse. If
    the comet is moving in an ellipse, the less its velocity, the less
    the eccentricity of its orbit: hence, in order to determine the form
    of the orbit of any comet, it is only necessary to ascertain its
    distance from the sun, and its velocity at any given time.

    Comets move in every direction in their orbits, and these orbits
    have every conceivable inclination to the ecliptic.

292. _Periodic Comets._--There are quite a number of comets which are
known to be _periodic_, returning to the sun at regular intervals in
elliptic orbits. Some of these have been observed at several returns, so
that their period has been determined with great certainty. In the case
of others the periodicity is inferred from the fact that the velocity
fell so far short of the parabolic limit that the comet must move in an
ellipse. The number of known periodic comets is increasing every year,
three having been added to the list in 1881.

The velocity of most comets is so near the parabolic limit that it is
not possible to decide, from observations, whether it falls short of it,
or exceeds it. In the case of a few comets the observations indicate a
minute excess of velocity; but this cannot be confidently asserted. It
is not, therefore, absolutely certain that any known comet revolves in a
hyperbolic orbit; and thus it is possible that all comets belong to our
system, and will ultimately return to it. It is, however, certain, that,
in the majority of cases, the return will be delayed for many centuries,
and perhaps for many thousand years.

293. _Origin of Comets._--It is now generally believed that the original
home of the comets is in the stellar spaces outside of our solar system,
and that they are drawn towards the sun, one by one, in the long lapse
of ages. Were the sun unaccompanied by planets, or were the planets
immovable, a comet thus drawn in would whirl around the sun in a
parabolic orbit, and leave it again never to return, unless its path
were again deflected by its approach to some star. But, when a comet is
moving in a parabola, the slightest _retardation_ would change its orbit
to an ellipse, and the slightest _acceleration_ into a hyperbola. Owing
to the motion of the several planets in their orbits, the velocity of a
comet would be changed on passing each of them. Whether its velocity
would be accelerated or retarded, would depend upon the way in which it
passed. Were the comet accelerated by the action of the planets, on its
passage through our system, more than it was retarded by them, it would
leave the system with a more than parabolic orbit, and would therefore
move in a hyperbola. Were it, on the contrary, retarded more than
accelerated by the action of the planets, its velocity would be reduced,
so that the comet would move in a more or less elongated ellipse, and
thus become a permanent member of the solar system.

In the majority of cases the retardation would be so slight that it
could not be detected by the most delicate observation, and the comet
would return to the sun only after the expiration of tens or hundreds of
thousands of years; but, were the comet to pass very near one of the
larger planets, the retardation might be sufficient to cause the comet
to revolve in an elliptical orbit of quite a short period. The orbit of
a comet thus captured by a planet would have its aphelion point near the
orbit of the planet which captured it. Now, it happens that each of the
larger planets has a family of comets whose aphelia are about its own
distance from the sun. It is therefore probable that these comets have
been captured by the action of these planets. As might be expected from
the gigantic size of Jupiter, the Jovian family of comets is the
largest. The orbits of several of the comets of this group are shown in
Fig. 324.

[Illustration: Fig. 324.]

294. _Number of Comets._--The number of comets recorded as visible to
the naked eye since the birth of Christ is about five hundred, while
about two hundred telescopic comets have been observed since the
invention of the telescope. The total number of comets observed since
the Christian era is therefore about seven hundred. It is certain,
however, that only an insignificant fraction of all existing comets have
ever been observed. Since they can be seen only when near their
perihelion, and since it is probable that the period of most of those
which have been observed is reckoned by thousands of years (if, indeed,
they ever return at all), our observations must be continued for many
thousand years before we have seen all which come within range of our
telescopes. Besides, as already stated (289), a comet can seldom be seen
unless its perihelion is either inside the orbit of the earth, or but
little outside of it; and it is probable that the perihelia of the great
majority of comets are beyond this limit of visibility.


                           Remarkable Comets.


295. _The Comet of 1680._--The great comet of 1680, shown in Fig. 320,
is one of the most celebrated on record. It was by his study of its
motions that Newton proved the orbit of a comet to be one of the conic
sections, and therefore that these bodies move under the influence of
gravity. This comet descended almost in a direct line to the sun,
passing nearer to that luminary than any comet before known. Newton
estimated, that, at its perihelion point, it was exposed to a
temperature two thousand times that of red-hot iron. During its
perihelion passage it was exceedingly brilliant. Halley suspected that
this comet had a period of five hundred and seventy-five years, and that
its first recorded appearance was in 43 B.C., its third in 1106, and its
fourth in 1680. If this is its real period, it will return in 2255. The
comet of 43 B.C. made its appearance just after the assassination of
Julius Cæsar. The Romans called it the _Julian Star_, and regarded it as
a celestial chariot sent to convey the soul of Cæsar to the skies. It
was seen two or three hours before sunset, and continued visible for
eight successive days. The great comet of 1106 was described as an
object of terrific splendor, and was visible in close proximity to the
sun. The comet of 1680 has become celebrated, not only on account of its
great brilliance, and on account of Newton's investigation of its orbit,
but also on account of the speculation of the theologian Whiston in
regard to it. He accepted five hundred and seventy-five years as its
period, and calculated that one of its earlier apparitions must have
occurred at the date of the flood, which he supposed to have been caused
by its near approach to the earth; and he imagined that the earth is
doomed to be destroyed by fire on some future encounter with this comet.

[Illustration: Fig. 325.]

296. _The Comet of 1811._--The great comet of 1811, a view of which is
given in Fig. 325, is, perhaps, the most remarkable comet on record. It
was visible for nearly seventeen months, and was very brilliant,
although at its perihelion passage it was over a hundred million miles
from the sun. Its tail was a hundred and twenty million miles in length,
and several million miles through. It has been calculated that its
aphelion point is about two hundred times as far from the sun as its
perihelion point, or some seven times the distance of Neptune from the
sun. Its period is estimated at about three thousand years. It was an
object of superstitious terror, especially in the East. The Russians
regarded it as presaging Napoleon's great and fatal war with Russia.

[Illustration: Fig. 326.]

[Illustration: Fig. 327.]

297. _Halley's Comet._--Halley's comet has become one of the most
celebrated of modern times. It is the first comet whose return was both
predicted and observed. It made its appearance in 1682. Halley computed
its orbit, and compared it with those of previous comets, whose orbits
he also computed from recorded observations. He found that it coincided
so exactly with that of the comet observed by Kepler in 1607, that there
could be no doubt of the identity of the two orbits. So close were they
together, that, were they both drawn in the heavens, the naked eye would
almost see them joined into one line. There could therefore be no doubt
that the comet of 1682 was the same that had appeared in 1607, and that
it moved in an elliptic orbit, with a period of about seventy-five
years. He found that this comet had previously appeared in 1531 and in
1456; and he predicted that it would return about 1758. Its actual
return was retarded somewhat by the action of the planets on it in its
passage through the solar system. It, however, appeared again in 1759,
and a third time in 1835. Its next appearance will be about 1911. The
orbit of this comet is shown in Fig. 326. Fig. 327 shows the comet as it
appeared to the naked eye, and in a telescope of moderate power, in
1835. This comet appears to be growing less brilliant. In 1456 it
appeared as a comet of great splendor; and coming as it did in a very
superstitious age, soon after the fall of Constantinople, and during the
threatened invasion of Europe by the Turks, it caused great alarm. Fig.
328 shows the changes undergone by the nucleus of this comet during its
perihelion passage in 1835.

[Illustration: Fig. 328.]

[Illustration: Fig. 329.]

[Illustration: Fig. 330.]

298. _Encke's Comet._--This telescopic comet, two views of which are
given in Figs. 329 and 330, appeared in 1818. Encke computed its orbit,
and found it to lie wholly within the orbit of Jupiter (Fig. 324), and
the period to be about three years and a third. By comparing the
intervals between the successive returns of this comet, it has been
ascertained that its orbit is continually growing smaller and smaller.
To account for the retardation of this comet, Olbers announced his
celebrated hypothesis, that the celestial spaces are filled with a
subtile _resisting medium_. This hypothesis was adopted by Encke, and
has been accepted by certain other astronomers; but it has by no means
gained universal assent.

299. _Biela's Comet._--This comet appeared in 1826, and was found to
have a period of about six years and two thirds. On its return in 1845,
it met with a singular, and as yet unexplained, accident, which has
rendered the otherwise rather insignificant comet famous. In November
and December of that year it was observed as usual, without any thing
remarkable about it; but, in January of the following year, it was found
to have been divided into two distinct parts, so as to appear as two
comets instead of one. The two parts were at first of very unequal
brightness; but, during the following month, the smaller of the two
increased in brilliancy until it equalled its companion; it then grew
fainter till it entirely disappeared, a month before its companion. The
two parts were about two hundred thousand miles apart. Fig. 331 shows
these two parts as they appeared on the 19th of February, and Fig. 332
as they appeared on the 21st of February. On its return in 1852, the
comets were found still to be double; but the two components were now
about a million and a half miles apart. They are shown in Fig. 333 as
they appeared at this time. Sometimes one of the parts appeared the
brighter, and sometimes the other; so that it was impossible to decide
which was really the principal comet. The two portions passed out of
view in September, and have not been seen since; although in 1872 the
position of the comet would have been especially favorable for
observation. The comet appears to have become completely broken up.

[Illustration: Fig. 331.]

[Illustration: Fig. 332.]

[Illustration: Fig. 333.]

[Illustration: Fig. 334.]

300. _The Comet of 1843._--The great comet of 1843, a view of which is
given in Fig. 334, was favorably situated for observation only in
southern latitudes. It was exceedingly brilliant, and was easily seen in
full daylight, in close proximity to the sun. The apparent length of its
tail was sixty-five degrees, and its real length a hundred and fifty
million miles, or nearly twice the distance from the earth to the sun.
This comet is especially remarkable on account of its near approach to
the sun. At the time of its perihelion passage the distance of the comet
from the photosphere of the sun was less than one-fourteenth of the
diameter of the sun. This distance was only one-half that of the comet
of 1680 when at its perihelion. When at perihelion, this comet was
plunging through the sun's outer atmosphere at the rate of one million,
two hundred and eighty thousand miles an hour. It passed half way round
the sun in the space of _two hours_, and its tail was whirled round
through a hundred and eighty degrees in that brief time. As the tail
extended almost double the earth's distance from the sun, the end of the
tail must have traversed in two hours a space nearly equal to the
circumference of the earth's orbit,--a distance which the earth, moving
at the rate of about twenty miles a second, is a _whole year_ in
passing. It is almost impossible to suppose that the matter forming this
tail remained the same throughout this tremendous sweep.

301. _Donati's Comet._--The great comet of 1858, known as _Donati's_
comet, was one of the most magnificent of modern times. When at its
brightest it was only about fifty million miles from the earth. Its tail
was then more than fifty million miles long. Had the comet at this time
been directly between the earth and sun, the earth must have passed
through its tail; but this did not occur. The orbit of this comet was
found to be decidedly elliptic, with a period of about two thousand
years. This comet is especially celebrated on account of the careful
telescopic observations of its nucleus and coma at the time of its
perihelion passage. Attention has already been called (287) to the
changes it underwent at that time. Its tail was curved, and of a curious
feather-like form, as shown in Fig. 335. At times it developed lateral
streamers, as shown in Fig. 336. Fig. 337 shows the head of the comet as
it was seen by Bond of the Harvard Observatory, whose delineations of
this comet have been justly celebrated.

[Illustration: Fig. 335.]

[Illustration: Fig. 336.]

[Illustration: Fig. 337.]

302. _The Comet of 1861._--The great comet of 1861 is remarkable for its
great brilliancy, for its peculiar fan-shaped tail, and for the probable
passage of the earth through its tail. Sir John Herschel declared that
it far exceeded in brilliancy any comet he had ever seen, not excepting
those of 1811 and 1858. Secchi found its tail to be a hundred and
eighteen degrees in length, the largest but one on record. Fig. 338
shows this comet as it appeared at one time. Fig. 339 shows the position
of the earth at _E_, in the tail of this comet, on the 30th of June,
1861. Fig. 340 shows the probable passage of the earth through the tail
of the comet on that date. As the tail of a comet doubtless consists of
something much less dense than our atmosphere, it is not surprising that
no noticeable effect was produced upon us by the encounter, if it
occurred.

[Illustration: Fig. 338.]

[Illustration: Fig. 339.]

[Illustration: Fig. 340.]

303. _Coggia's Comet._--This comet, which appeared in 1874, looked very
large, because it came very near the earth. It was not at all brilliant.
Its nucleus was carefully studied, and was found to develop a series of
envelops similar to those of Donati's comet. Figs. 341 and 342 are two
views of the head of this comet. Fig. 343 shows the system of envelops
that were developed during its perihelion passage.

[Illustration: Fig. 341.]

[Illustration: Fig. 342.]

[Illustration: Fig. 343.]

304. _The Comet of June, 1881._--This comet, though far from being one
of the largest of modern times, was still very brilliant. It will ever
be memorable as the first brilliant comet which has admitted of careful
examination with the spectroscope.


                 Connection between Meteors and Comets.


305. _Shooting-Stars._--On watching the heavens any clear night, we
frequently see an appearance as of a star shooting rapidly through a
short space in the sky, and then suddenly disappearing. Three or four
such _shooting-stars_ may, on the average, be observed in the course of
an hour. They are usually seen only a second or two; but they sometimes
move slowly, and are visible much longer. These stars begin to be
visible at an average height of about seventy-five miles, and they
disappear at an average height of about fifty miles. They are
occasionally seen as high as a hundred and fifty miles, and continue to
be visible till within thirty miles of the earth. Their visible paths
vary from ten to a hundred miles in length, though they are occasionally
two hundred or three hundred miles long. Their average velocity,
relatively to the earth's surface, varies from ten to forty-five miles a
second.

The average number of shooting-stars visible to the naked eye at any one
place is estimated at about _a thousand an hour_; and the average number
large enough to be visible to the naked eye, that traverse the
atmosphere daily, is estimated at _over eight millions_. The number of
telescopic shooting-stars would of course be much greater.

Occasionally, shooting-stars leave behind them a trail of light which
lasts for several seconds. These trails are sometimes straight, as shown
in Fig. 344, and sometimes curved, as in Figs. 345 and 346. They often
disappear like trails of smoke, as shown in Fig. 347.

[Illustration: Fig. 344.]

[Illustration: Fig. 345.]

[Illustration: Fig. 346.]

[Illustration: Fig. 347.]

Shooting-stars are seen to move in all directions through the heavens.
Their apparent paths are, however, generally inclined downward, though
sometimes upward; and after midnight they come in the greatest numbers
from that quarter of the heavens toward which the earth is moving in its
journey around the sun.

306. _Meteors._--Occasionally these bodies are brilliant enough to
illuminate the whole heavens. They are then called _meteors_, although
this term is equally applicable to ordinary shooting-stars. Such a
meteor is shown in Fig. 348.

[Illustration: Fig. 348.]

Sometimes these brilliant meteors are seen to explode, as shown in Fig.
349; and the explosion is accompanied with a loud detonation, like the
discharge of cannon.

[Illustration: Fig. 349.]

Ordinary shooting-stars are not accompanied by any audible sound, though
they are sometimes seen to break in pieces. Meteors which explode with
an audible sound are called _detonating meteors_.

307. _Aerolites._--There is no certain evidence that any deposit from
ordinary shooting-stars ever reaches the surface of the earth; though a
peculiar dust has been found in certain localities, which has been
supposed to be of meteoric origin, and which has been called _meteoric
dust_. But solid bodies occasionally descend to the earth from beyond
our atmosphere. These generally penetrate a foot or more into the earth,
and, if picked up soon after their fall, are found to be warm, and
sometimes even hot. These bodies are called _aerolites_. When they have
a stony appearance, and contain but little iron, they are called
_meteoric stones_; when they have a metallic appearance, and are
composed largely of iron, they are called _meteoric iron_.

There are eighteen well-authenticated cases in which aerolites have
fallen in the United States during the last sixty years, and their
aggregate weight is twelve hundred and fifty pounds. The entire number
of known aerolites the date of whose fall is well determined is two
hundred and sixty-one. There are also on record seventy-four cases of
which the date is more or less uncertain. There have also been found
eighty-six masses, which, from their peculiar composition, are believed
to be aerolites, though their fall was not seen. The weight of these
masses varies from a few pounds to several tons. The entire number of
aerolites of which we have any knowledge is therefore about four hundred
and twenty.

Aerolites are composed of the same elementary substances as occur in
terrestrial minerals, not a single new element having been found in
their analysis. Of the sixty or more elements now recognized by
chemists, about twenty have been found in aerolites.

While aerolites contain no new elements, their appearance is quite
peculiar; and the compounds found in them are so peculiar as to enable
us by chemical analysis to distinguish an aerolite from any terrestrial
substance.

Iron ores are very abundant in nature, but iron in the metallic state is
exceedingly rare. Now, aerolites invariably contain metallic iron,
sometimes from ninety to ninety-six per cent. This iron is malleable,
and may be readily worked into cutting instruments. It always contains
eight or ten per cent of nickel, together with small quantities of
cobalt, copper, tin, and chromium. This composition _has never been
found in any terrestrial mineral_. Aerolites also contain, usually in
small amount, a compound of iron, nickel, and phosphorus, which has
never been found elsewhere.

Meteorites often present the appearance of having been fused on the
surface to a slight depth, and meteoric iron is found to have a peculiar
crystalline structure. The external appearance of a piece of meteoric
iron found near Lockport, N.Y., is shown in Fig. 350. Fig. 351 shows the
peculiar internal structure of meteoric iron.

[Illustration: Fig. 350.]

[Illustration: Fig. 351.]

308. _Meteoroids._--Astronomers now universally hold that
shooting-stars, meteors, and aerolites are all minute bodies, revolving,
like the comets, about the sun. They are moving in every possible
direction through the celestial spaces. They may not average more than
one in a million of cubic miles, and yet their total number exceeds all
calculation. Of the nature of the minuter bodies of this class nothing
is certainly known. The earth is continually encountering them in its
journey around the sun. They are burned by passing through the upper
regions of our atmosphere, and the shooting-star is simply the light of
that burning. These bodies, which are invisible till they plunge into
the earth's atmosphere, are called _meteoroids_.

309. _Origin of the Light of Meteors._--When one of these meteoroids
enters our atmosphere, the resistance of the air arrests its motion to
some extent, and so converts a portion of its energy of motion into that
of heat. The heat thus developed is sufficient to raise the meteoroid
and the air around it to incandescence, and in most cases either to
cause the meteoroid to burn up, or to dissipate it as vapor. The
luminous vapor thus formed constitutes the luminous train which
occasionally accompanies a meteor, and often disappears as a puff of
smoke. When a meteoroid is large enough and refractory enough to resist
the heat to which it is exposed, its motion is sufficiently arrested, on
entering the lower layers of our atmosphere, to cause it to fall to the
earth. We then have an _aerolite_. A brilliant meteor differs from a
shooting-star simply in magnitude.

310. _The Intensity of the Heat to which a Meteoroid is Exposed._--It
has been ascertained by experiment that a body moving through the
atmosphere at the rate of a hundred and twenty-five feet a second raises
the temperature of the air immediately in front of it one degree, and
that the temperature increases as the square of the velocity of the
moving body; that is to say, that, with a velocity of two hundred and
fifty feet, the temperature in front of the body would be raised four
degrees; with a velocity of five hundred feet, sixteen degrees; and so
on. To find, therefore, the temperature to which a meteoroid would be
exposed in passing through our atmosphere, we have merely to divide its
velocity in feet per second by a hundred and twenty-five, and square the
quotient. With a velocity of forty-four miles a second in our
atmosphere, a meteoroid would therefore be exposed to a temperature of
between three and four million degrees. The air acts upon the body as if
it were raised to this intense heat. At such a temperature small masses
of the most refractory or incombustible substances known to us would
flash into vapor with the evolution of intense light and heat.

If one of these meteoric bodies is large enough to pass through the
atmosphere and reach the earth, without being volatilized by the heat,
we have an aerolite. As it is only a few seconds in making the passage,
the heat has not time to penetrate far into its interior, but is
expended in melting and vaporizing the outer portions. The resistance of
the denser strata of the atmosphere to the motion of the aerolite
sometimes becomes so enormous that the body is suddenly rent to pieces
with a loud detonation. It seems like an explosion produced by some
disruptive action within the mass; but there can be little doubt that it
is due to the velocity--perhaps ten, twenty, or thirty miles a
second--with which the body strikes the air.

If, on the other hand, the meteoroid is so small as to be burned up or
volatilized in the upper regions of the atmosphere, we have a common
shooting-star, or a meteor of greater or less brilliancy.

[Illustration: Fig. 352.]

311. _Meteoric Showers._--On ordinary nights only four or five
shooting-stars are seen in an hour, and these move in every direction.
Their orbits lie in all possible positions, and are seemingly scattered
at random. Such meteors are called _sporadic_ meteors. On occasional
nights, shooting-stars are more numerous, and all move in a common
direction. Such a display is called a _meteoric shower_. These showers
differ greatly in brilliancy; but during any one shower the meteors all
appear to radiate from some one point in the heavens. If we mark on a
celestial globe the apparent paths of the meteors which fall during a
shower, or if we trace them back on the celestial sphere, we shall find
that they all meet in the same point, as shown in Fig. 352. This point
is called the _radiant point_. It always appears in the same position,
wherever the observer is situated, and does not partake of the diurnal
motion of the earth. As the stars move towards the west, the radiant
point moves with them. The point in question is purely an effect of
perspective, being the "vanishing point" of the parallel lines in which
the meteors are actually moving. These lines are seen, not in their real
direction in space, but as projected on the celestial sphere. If we look
upwards, and watch snow falling through a calm atmosphere, the flakes
which fall directly towards us do not seem to move at all, while the
surrounding flakes seem to diverge from them on all sides. So, in a
meteoric shower, a meteor coming directly towards the observer does not
seem to move at all, and marks the point from which all the others seem
to radiate.

312. _The August Meteors._--A meteoric shower of no great brilliancy
occurs annually about the 10th of August. The radiant point of this
shower is in the constellation _Perseus_, and hence these meteors are
often called the _Perseids_. The orbit of these meteoroids has been
pretty accurately determined, and is shown in Fig. 353.

[Illustration: Fig. 353.]

It will be seen that the perihelion point of this orbit is at about the
distance of the earth from the sun; so that the earth encounters the
meteors once a year, and this takes place in the month of August. The
orbit is a very eccentric ellipse, reaching far beyond Neptune. As the
meteoric display is about equally brilliant every year, it seems
probable that the meteoroids form a stream quite uniformly distributed
throughout the whole orbit. It probably takes one of the meteoroids
about a hundred and twenty-four years to pass around this orbit.

[Illustration: Fig. 354.]

313. _The November Meteors._--A somewhat brilliant meteoric shower also
occurs annually, about the 13th of November. The radiant point of these
meteors is in the constellation _Leo_, and hence they are often called
the _Leonids_. Their orbit has been determined with great accuracy, and
is shown in Fig. 354. While the November meteors are not usually very
numerous or bright, a remarkably brilliant display of them has been seen
once in about thirty-three or thirty-four years: hence we infer, that,
while there are some meteoroids scattered throughout the whole extent of
the orbit, the great majority are massed in a group which traverses the
orbit in a little over thirty-three years. A conjectural form of this
condensed group is shown in Fig. 355. The group is so large that it
takes it two or three years to pass the perihelion point: hence there
may be a brilliant meteoric display two or three years in succession.

[Illustration: Fig. 355.]

The last brilliant display of these meteors was in the years 1866 and
1867. The display was visible in this country only a short time before
sunrise, and therefore did not attract general attention. The display of
1833 was remarkably brilliant in this country, and caused great
consternation among the ignorant and superstitious.

[Illustration: Fig. 356.]

314. _Connection between Meteors and Comets._--It has been found that a
comet which appeared in 1866, and which is designated as 1866, I., has
exactly the same orbit and period as the November meteors, and that
another comet, known as the 1862, III., has the same orbit as the August
meteors. It has also been ascertained that a third comet, 1861, I., has
the same orbit as a stream of meteors which the earth encounters in
April. Furthermore, it was found, in 1872, that there was a small stream
of meteors following in the train of the lost comet of Biela. These
various orbits of comets and meteoric streams are shown in Fig. 356. The
coincidence of the orbits of comets and of meteoric streams indicates
that these two classes of bodies are very closely related. They
undoubtedly have a common origin. The fact that there is a stream of
meteors in the train of Biela's comet has led to the supposition that
comets may become gradually disintegrated into meteoroids.


             Physical and Chemical Constitution of Comets.


315. _Physical Constitution of Telescopic Comets._--We have no certain
knowledge of the physical constitution of telescopic comets. They are
usually tens of thousands of miles in diameter, and yet of such tenuity
that the smallest stars can readily be seen through them. It would seem
that they must shine in part by reflected light; yet the spectroscope
shows that their spectrum is composed of bright bands, which would
indicate that they are composed, in part at least, of incandescent
gases. It is, however, difficult to conceive how these gases become
sufficiently heated to be luminous; and at the same time such gases
would reflect no sunlight.

It seems probable that these comets are really made up of a combination
of small, solid particles in the form of minute meteoroids, and of gases
which are, perhaps, rendered luminous by electric discharges of slight
intensity.

316. _Physical Constitution of Large Comets._--In the case of large
comets the nucleus is either a dense mass of solid matter several
hundred miles in diameter, or a dense group of meteoroids. Professor
Peirce estimated that the density of the nucleus is at least equal to
that of iron. As such a comet approaches the sun, the nucleus is, to a
slight extent, vaporized, and out of this vapor is formed the coma and
the tail.

That some evaporating process is going on from the nucleus of the comet
is proved by the movements of the tail. It is evident that the tail
cannot be an appendage carried along with the comet, as it seems to be.
It is impossible that there should be any cohesion in matter of such
tenuity that the smallest stars could be seen through a million of miles
of it, and which is, moreover, continually changing its form. Then,
again, as a comet is passing its perihelion, the tail appears to be
whirled from one side of the sun to another with a rapidity which would
tear it to pieces if the movement were real. The tail seems to be, not
something attached to the comet, and carried along with it, but a stream
of vapor issuing from it, like smoke from a chimney. The matter of which
it is composed is continually streaming outwards, and continually being
replaced by fresh vapor from the nucleus.

The vapor, as it emanates from the nucleus, is repelled by the sun with
a force often two or three times as great as the ordinary solar
attraction. The most probable explanation of this phenomenon is, that it
is a case of electrical repulsion, the sun and the particles of the
cometary mist being similarly electrified. With reference to this
electrical theory of the formation of comets' tails, Professor Peirce
makes the following observation: "In its approach to the sun, the
surface of the nucleus is rapidly heated: it is melted and vaporized,
and subjected to frequent explosions. The vapor rises in its atmosphere
with a well-defined upper surface, which is known to observers as an
_envelop_.... The electrification of the cometary mist is analogous to
that of our own thunder-clouds. Any portion of the coma which has
received the opposite kind of electricity to the sun and to the repelled
tail will be attracted. This gives a simple explanation of the negative
tails which have been sometimes seen directed towards the sun. In cases
of violent explosion, the whole nucleus might be broken to pieces, and
the coma dashed around so as to give varieties of tail, and even
multiple tails. There seems, indeed, to be no observed phenomenon of the
tail or the coma which is not consistent with a reasonable modification
of the theory." Professor Peirce regarded comets simply as the largest
of the meteoroids. They appear to shine partly by reflected sunlight,
and partly by their own proper light, which seems to be that of vapor
rendered luminous by an electric discharge of slight intensity.

[Illustration: Fig. 357.]

317. _Collision of a Comet and the Earth._--It sometimes happens that
the orbit of a comet intersects that of the earth, as is shown in Fig.
357, which shows a portion of the orbit of Biela's comet, with the
positions of the comet and of the earth in 1832. Of course, were a comet
and the earth both to reach the intersection of their orbits at the same
time, a collision of the two bodies would be inevitable. With reference
to the probable effect of such a collision, Professor Newcomb remarks,--

"The question is frequently asked, What would be the effect if a comet
should strike the earth? This would depend upon what sort of a comet it
was, and what part of the comet came in contact with our planet. The
latter might pass through the tail of the largest comet without the
slightest effect being produced; the tail being so thin and airy that a
million miles thickness of it looks only like gauze in the sunlight. It
is not at all unlikely that such a thing may have happened without ever
being noticed. A passage through a telescopic comet would be accompanied
by a brilliant meteoric shower, probably a far more brilliant one than
has ever been recorded. No more serious danger would be encountered than
that arising from a possible fall of meteorites; but a collision between
the nucleus of a large comet and the earth might be a serious matter.
If, as Professor Peirce supposes, the nucleus is a solid body of
metallic density, many miles in diameter, the effect where the comet
struck would be terrific beyond conception. At the first contact in the
upper regions of the atmosphere, the whole heavens would be illuminated
with a resplendence beyond that of a thousand suns, the sky radiating a
light which would blind every eye that beheld it, and a heat which would
melt the hardest rocks. A few seconds of this, while the huge body was
passing through the atmosphere, and the collision at the earth's surface
would in an instant reduce everything there existing to fiery vapor, and
bury it miles deep in the solid earth. Happily, the chances of such a
calamity are so minute that they need not cause the slightest
uneasiness. There is hardly a possible form of death which is not a
thousand times more probable than this. So small is the earth in
comparison with the celestial spaces, that if one should shut his eyes,
and fire a gun at random in the air, the chance of bringing down a bird
would be better than that of a comet of any kind striking the earth."

[Illustration: Fig. 358.]

[Illustration: Fig. 359.]

318. _The Chemical Constitution of Comets._--Fig. 358 shows the bands of
the spectrum of a telescopic comet of 1873, as seen by two different
observers. Fig. 359 shows the spectrum of the coma and tail of the comet
of 1874; and the spectrum of the bright comet of 1881 showed the same
three bands for the coma and tail. Now, these three bands are those of
certain hydrocarbon vapors: hence it would seem that the coma and tails
of comets are composed chiefly of such vapors (315).


                        II. THE ZODIACAL LIGHT.


319. _The General Appearance of the Zodiacal Light._--The phenomenon
known as the _zodiacal light_ consists of a very faint luminosity, which
may be seen rising from the western horizon after twilight on any clear
winter or spring evening, also from the eastern horizon just before
daybreak in the summer or autumn. It extends out on each side of the
sun, and lies nearly in the plane of the ecliptic. It grows fainter the
farther it is from the sun, and can generally be traced to about ninety
degrees from that luminary, when it gradually fades away. In a very
clear, tropical atmosphere, it has been traced all the way across the
heavens from east to west, thus forming a complete ring. The general
appearance of this column of light, as seen in the morning, in the
latitude of Europe, is shown in Fig. 360.

[Illustration: Fig. 360.]

Taking all these appearances together, they indicate that it is due to a
lens-shaped appendage surrounding the sun, and extending a little beyond
the earth's orbit. It lies nearly in the plane of the ecliptic; but its
exact position is not easily determined. Fig. 361 shows the general form
and position of this solar appendage, as seen in the west.

[Illustration: Fig. 361.]

320. _The Visibility of the Zodiacal Light._--The reason why the
zodiacal light is more favorably seen in the evening during the winter
and spring than in the summer and fall is evident from Fig. 362, which
shows the position of the ecliptic and the zodiacal light with reference
to the western horizon at the time of sunset in March and in September.
It will be seen that in September the axis of the light forms a small
angle with the horizon, so that the phenomenon is visible only a short
time after sunset and low down where it is difficult to distinguish it
from the glimmer of the twilight; while in March, its axis being nearly
perpendicular to the horizon, the light may be observed for some hours
after sunset and well up in the sky. Fig. 363 gives the position of the
ecliptic and of the zodiacal light with reference to the eastern horizon
at the time of sunrise, and shows why the zodiacal light is seen to
better advantage in the morning during the summer and fall than during
the winter and spring. It will be observed that here the angle made by
the axis of the light with the horizon is small in March, while it is
large in September; the conditions represented in the preceding figure
being thus reversed.

[Illustration: Fig. 362.]

[Illustration: Fig. 363.]

321. _Nature of the Zodiacal Light._--Various attempts have been made to
explain the phenomena of the zodiacal light; but the most probable
theory is, that it is due to an immense number of meteors which are
revolving around the sun, and which lie mostly within the earth's orbit.
Each of these meteors reflects a sensible portion of sunlight, but is
far too small to be separately visible. All of these meteors together
would, by their combined reflection, produce a kind of pale, diffused
light.




                       III. THE STELLAR UNIVERSE.


                   I. GENERAL ASPECT OF THE HEAVENS.


322. _The Magnitude of the Stars._--The stars that are visible to the
naked eye are divided into six classes, according to their brightness.
The brightest stars are called stars of the _first magnitude_; the next
brightest, those of the _second magnitude_; and so on to the _sixth
magnitude_. The last magnitude includes the faintest stars that are
visible to the naked eye on the most favorable night. Stars which are
fainter than those of the sixth magnitude can be seen only with the
telescope, and are called _telescopic stars_. Telescopic stars are also
divided into magnitudes; the division extending to the _sixteenth_
magnitude, or the faintest stars that can be seen with the most powerful
telescopes.

The classification of stars according to magnitudes has reference only
to their brightness, and not at all to their actual size. A sixth
magnitude star may actually be larger than a first magnitude star; its
want of brilliancy being due to its greater distance, or to its inferior
luminosity, or to both of these causes.

None of the stars present any sensible disk, even in the most powerful
telescope: they all appear as mere points of light. The larger the
telescope, the greater is its power of revealing faint stars; not
because it makes these stars appear larger, but because of its greater
light-gathering power. This power increases with the size of the
object-glass of the telescope, which plays the part of a gigantic pupil
of the eye.

The classification of the stars into magnitudes is not made in
accordance with any very accurate estimate of their brightness. The
stars which are classed together in the same magnitude are far from
being equally bright.

The stars of each lower magnitude are about two-fifths as bright as
those of the magnitude above. The ratio of diminution is about a third
from the higher magnitude down to the fifth. Were the ratio two-fifths
exact, it would take about

            2-1/2 stars of the 2d magnitude to make one of the 1st.
            6     stars of the 3d magnitude to make one of the 1st.
           16     stars of the 4th magnitude to make one of the 1st.
           40     stars of the 5th magnitude to make one of the 1st.
          100     stars of the 6th magnitude to make one of the 1st.
       10,000     stars of the 11th magnitude to make one of the 1st.
    1,000,000     stars of the 16th magnitude to make one of the 1st.

323. _The Number of the Stars._--The total number of stars in the
celestial sphere visible to the average naked eye is estimated, in round
numbers, at five thousand; but the number varies much with the
perfection and the training of the eye and with the atmospheric
conditions. For every star visible to the naked eye, there are thousands
too minute to be seen without telescopic aid. Fig. 364 shows a portion
of the constellation of the Twins as seen with the naked eye; and Fig.
365 shows the same region as seen in a powerful telescope.

[Illustration: Fig. 364.]

[Illustration: Fig. 365.]

Struve has estimated that the total number of stars visible with
Herschel's twenty-foot telescope was about twenty million. The number
that can be seen with the great telescopes of modern times has not been
carefully estimated, but is probably somewhere between thirty million
and fifty million.

The number of stars between the north pole and the circle thirty-five
degrees south of the equator is about as follows:--

    Of the 1st magnitude about        14 stars.
    Of the 2d magnitude about         48 stars.
    Of the 3d magnitude about        152 stars.
    Of the 4th magnitude about       313 stars.
    Of the 5th magnitude about       854 stars.
    Of the 6th magnitude about      2010 stars.
                                    ----
    Total visible to naked eye      3391 stars.

The number of stars of the several magnitudes is approximately in
inverse proportion to that of their brightness, the ratio being a little
greater in the higher magnitudes, and probably a little less in the
lower ones.

324. _The Division of the Stars into Constellations._--A glance at the
heavens is sufficient to show that the stars are not distributed
uniformly over the sky. The larger ones especially are collected into
more or less irregular groups. The larger groups are called
_constellations_. At a very early period a mythological figure was
allotted to each constellation; and these figures were drawn in such a
way as to include the principal stars of each constellation. The heavens
thus became covered, as it were, with immense hieroglyphics.

There is no historic record of the time when these figures were formed,
or of the principle in accordance with which they were constructed. It
is probable that the imagination of the earlier peoples may, in many
instances, have discovered some fanciful resemblance in the
configuration of the stars to the forms depicted. The names are still
retained, although the figures no longer serve any astronomical purpose.
The constellation Hercules, for instance, no longer represents the
figure of a man among the stars, but a certain portion of the heavens
within which the ancients placed that figure. In star-maps intended for
school and popular use it is still customary to give these figures; but
they are not generally found on maps designed for astronomers.

325. _The Naming of the Stars._--The brighter stars have all proper
names, as _Sirius_, _Procyon_, _Arcturus_, _Capella_, _Aldebaran_, etc.
This method of designating the stars was adopted by the Arabs. Most of
these names have dropped entirely out of astronomical use, though many
are popularly retained. The brighter stars are now generally designated
by the letters of the Greek alphabet,--_alpha_, _beta_, _gamma_,
etc.,--to which is appended the genitive of the name of the
constellation, the first letter of the alphabet being used for the
brightest star, the second for the next brightest, and so on. Thus
_Aldebaran_ would be designated as _Alpha Tauri_. In speaking of the
stars of any one constellation, we simply designate them by the letters
of the Greek alphabet, without the addition of the name of the
constellation, which answers to a person's surname, while the Greek
letter answers to his Christian name. The names of the seven stars of
the "Dipper" are given in Fig. 366. When the letters of the Greek
alphabet are exhausted, those of the Roman alphabet are employed. The
fainter stars in a constellation are usually designated by some system
of numbers.

[Illustration: Fig. 366.]

326. _The Milky-Way, or Galaxy._--The Milky-Way is a faint luminous
band, of irregular outline, which surrounds the heavens with a great
circle, as shown in Fig. 367. Through a considerable portion of its
course it is divided into two branches, and there are various vacant
spaces at different points in this band; but at only one point in the
southern hemisphere is it entirely interrupted.

[Illustration: Fig. 367.]

The telescope shows that the Galaxy arises from the light of countless
stars too minute to be separately visible with the naked eye. The
telescopic stars, instead of being uniformly distributed over the
celestial sphere, are mostly condensed in the region of the Galaxy. They
are fewest in the regions most distant from this belt, and become
thicker as we approach it. The greater the telescopic power, the more
marked is the condensation. With the naked eye the condensation is
hardly noticeable; but with the aid of a very small telescope, we see a
decided thickening of the stars in and near the Galaxy, while the most
powerful telescopes show that a large majority of the stars lie actually
in the Galaxy. If all the stars visible with a twelve-inch telescope
were blotted out, we should find that the greater part of those
remaining were in the Galaxy.

[Illustration: Fig. 368.]

The increase in the number of the stars of all magnitudes as we approach
the plane of the Milky-Way is shown in Fig. 368. The curve _acb_ shows
by its height the distribution of the stars above the ninth magnitude,
and the curve _ACB_ those of all magnitudes.

327. _Star-Clusters._--Besides this gradual and regular condensation
towards the Galaxy, occasional aggregations of stars into _clusters_ may
be seen. Some of these are visible to the naked eye, sometimes as
separate stars, like the "Seven Stars," or Pleiades, but more commonly
as patches of diffused light, the stars being too small to be seen
separately. The number visible in powerful telescopes is, however, much
greater. Sometimes hundreds or even thousands of stars are visible in
the field of view at once, and sometimes the number is so great that
they cannot be counted.

328. _Nebulæ._--Another class of objects which are found in the
celestial spaces are irregular masses of soft, cloudy light, known as
_nebulæ_. Many objects which look like nebulæ in small telescopes are
shown by more powerful instruments to be really star-clusters. But many
of these objects are not composed of stars at all, being immense masses
of gaseous matter.

[Illustration: Fig. 369.]

The general distribution of nebulæ is the reverse of that of the stars.
Nebulæ are thickest where stars are thinnest. While stars are most
numerous in the region of the Milky-Way, nebulæ are most abundant about
the poles of the Milky-Way. This condensation of nebulæ about the poles
of the Milky-Way is shown in Figs. 367 and 369, in which the points
represent, not stars, but nebulæ.


                             II. THE STARS.


                          The Constellations.


[Illustration: Fig. 370.]

[Illustration: Fig. 371.]

329. _The Great Bear._--The Great Bear, or _Ursa Major_, is one of the
circumpolar constellations (4), and contains one of the most familiar
_asterisms_, or groups of stars, in our sky; namely, the _Great Dipper_,
or _Charles's Wain_. The positions and names of the seven prominent
stars in it are shown in Fig. 370. The two stars Alpha and Beta are
called the _Pointers_. This asterism is sometimes called the _Butcher's
Cleaver_. The whole constellation is shown in Fig. 371. A rather faint
star marks the nose of the bear, and three equidistant pairs of faint
stars mark his feet.

330. _The Little Bear, Draco, and Cassiopeia._--These are all
circumpolar constellations. The most important star of the Little Bear,
or _Ursa Minor_, is _Polaris_, or the _Pole Star_. This star may be
found by drawing a line from Beta to Alpha of the Dipper, and prolonging
it as shown in Fig. 372. This explains why these stars are called the
_Pointers_. The Pole Star, with the six other chief stars of the Little
Bear, form an asterism called the _Little Dipper_. These six stars are
joined with Polaris by a dotted line in Fig. 372.

[Illustration: Fig. 372.]

The stars in a serpentine line between the two Dippers are the chief
stars of _Draco_, or the _Dragon_; the trapezium marking its head. Fig.
373 shows the constellations of Ursa Minor and Draco as usually figured.

[Illustration: Fig. 373.]

To find _Cassiopeia_, draw a line from Delta of the Dipper to Polaris,
and prolong it about an equal distance beyond, as shown in Fig. 372.
This line will pass near Alpha of Cassiopeia. The five principal stars
of this constellation form an irregular _W_, opening towards the pole.
Between Cassiopeia and Draco are five rather faint stars, which form an
irregular _K_. These are the principal stars of the constellation
_Cepheus_. These two constellations are shown in Fig. 374.

[Illustration: Fig. 374.]

[Illustration: Fig. 375.]

331. _The Lion, Berenice's Hair, and the Hunting-Dogs._--A line drawn
from Alpha to Beta of the Dipper, and prolonged as shown in Fig. 375,
will pass between the two stars _Denebola_ and _Regulus_ of _Leo_, or
the _Lion_. Regulus forms a _sickle_ with several other faint stars, and
marks the heart of the lion. Denebola is at the apex of a right-angled
triangle, which it forms with two other stars, and marks the end of the
lion's tail. This constellation is visible in the evening from February
to July, and is figured in Fig. 376.

[Illustration: Fig. 376.]

In a straight line between Denebola and Eta, at the end of the Great
Bear's tail, are, at about equal distances, the two small constellations
of _Coma Berenices_, or _Berenice's Hair_, and _Canes Venatici_, or the
_Hunting-Dogs_. These are shown in Fig. 377. The dogs are represented as
pursuing the bear, urged on by the huntsman _Boötes_.

[Illustration: Fig. 377.]

332. _Boötes, Hercules, and the Northern Crown._--_Arcturus_, the
principal star of _Boötes_, may be found by drawing a line from Zeta to
Eta of the Dipper, and then prolonging it with a slight bend, as shown
in Fig. 378. Arcturus and Polaris form a large isosceles triangle with a
first-magnitude star called _Vega_. This triangle encloses at one corner
the principal stars of Boötes, and the head of the Dragon near the
opposite side. The side running from Arcturus to Vega passes through
_Corona Borealis_, or the _Northern Crown_, and the body of _Hercules_,
which is marked by a quadrilateral of four stars.

[Illustration: Fig. 378.]

_Boötes_, who is often represented as a husbandman, _Corona Borealis_,
and _Hercules_, are delineated in Fig. 379. These constellations are
visible in the evening from May to September.

[Illustration: Fig. 379.]

[Illustration: Fig. 380.]

333. _The Lyre, the Swan, the Eagle, and the Dolphin._--_Altair_, the
principal star of _Aquila_, or the _Eagle_, lies on the opposite side of
the Milky-Way from Vega. Altair is a first-magnitude star, and has a
faint star on each side of it, as shown in Fig. 380. Vega, also of the
first magnitude, is the principal star of _Lyra_, or the _Lyre_. Between
these two stars, and a little farther to the north, are several stars
arranged in the form of an immense cross. The bright star at the head of
this cross is called _Deneb_. The cross lies in the Milky-Way, and
contains the chief stars of the constellation _Cygnus_, or the _Swan_. A
little to the north of Altair are four stars in the form of a diamond.
This asterism is popularly known as _Job's Coffin_. These four stars are
the chief stars of _Delphinus_, or the _Dolphin_. These four
constellations are shown together in Fig. 381. The _Swan_ is visible
from June to December, in the evening.

[Illustration: Fig. 381.]

334. _Virgo._--A line drawn from Alpha to Gamma of the Dipper, and
prolonged with a slight bend at Gamma, will reach to a first-magnitude
star called _Spica_ (Fig. 382). This is the chief star of the
constellation _Virgo_, or the _Virgin_, and forms a large isosceles
triangle with _Arcturus_ and _Denebola_.

[Illustration: Fig. 382.]

_Virgo_ is represented in Fig. 383. To the right of this constellation,
as shown in the figure, there are four stars which form a trapezium, and
mark the constellation _Corvus_, or the _Crow_. This bird is represented
as standing on the body of _Hydra_, or the _Water-Snake_. _Virgo_ is
visible in the evening, from April to August.

[Illustration: Fig. 383.]

[Illustration: Fig. 384.]

[Illustration: Fig. 385.]

335. _The Twins._--A line drawn from Delta to Beta of the Dipper, and
prolonged as shown in Fig. 384, passes between two bright stars called
_Castor_ and _Pollux_. The latter of these is usually reckoned as a
first-magnitude star. These are the principal stars of the constellation
_Gemini_, or the _Twins_, which is shown in Fig. 385. The constellation
_Canis Minor_, or the _Little Dog_, is shown in the lower part of the
figure. There are two conspicuous stars in this constellation, the
brightest of which is of the first magnitude, and called _Procyon_.

The region to which we have now been brought is the richest of the
northern sky, containing no less than seven first-magnitude stars. These
are _Sirius_, _Procyon_, _Pollux_, _Capella_, _Aldebaran_, _Betelgeuse_,
and _Rigel_. They are shown in Fig. 386.

[Illustration: Fig. 386.]

_Betelgeuse_ and _Rigel_ are in the constellation _Orion_, being about
equally distant to the north and south from the three stars forming the
_belt_ of Orion. Betelgeuse is a red star. _Sirius_ is the brightest
star in the heavens, and belongs to the constellation _Canis Major_, or
the _Great Dog_. It lies to the east of the belt of Orion. _Aldebaran_
lies at about the same distance to the west of the belt. It is a red
star, and belongs to the constellation _Taurus_, or the _Bull_.
_Capella_ is in the constellation _Auriga_, or the _Wagoner_. These
stars are visible in the evening, from about December to April.

336. _Orion and his Dogs, and Taurus._--_Orion_ and his _Dogs_ are shown
in Fig. 387, and _Orion_ and _Taurus_ in Fig. 388. _Aldebaran_ marks one
of the eyes of the bull, and is often called the _Bull's Eye_. The
irregular _V_ in the face of the bull is called the _Hyades_, and the
cluster on the shoulder the _Pleiades_.

[Illustration: Fig. 387.]

[Illustration: Fig. 388.]

[Illustration: Fig. 389.]

337. _The Wagoner._--The constellation _Auriga_, or the _Wagoner_
(sometimes called the _Charioteer_), is shown in Fig. 389. _Capella_
marks the _Goat_, which he is represented as carrying on his back, and
the little right-angled triangle of stars near it the _Kids_. The five
chief stars of this constellation form a large, irregular pentagon.
Gamma of _Auriga_ is also Beta of _Taurus_, and marks one of the horns
of the _Bull_.

[Illustration: Fig. 390.]

338. _Pegasus, Andromeda, and Perseus._--A line drawn from Polaris near
to Beta of _Cassiopeia_ will lead to a bright second-magnitude star at
one corner of a large square (Fig. 390). Alpha belongs both to the
_Square of Pegasus_ and to _Andromeda_. Beta and Gamma, which are
connected with Alpha in the figure by a dotted line, also belong to
Andromeda. _Algol_, which forms, with the last-named stars and with the
_Square of Pegasus_, an asterism similar in configuration to the _Great
Dipper_, belongs to _Perseus_. _Algenib_, which is reached by bending
the line at Gamma in the opposite direction, is the principal star of
_Perseus_.

[Illustration: Fig. 391.]

[Illustration: Fig. 392.]

[Illustration: Fig. 393.]

_Pegasus_ is shown in Fig. 391, and _Andromeda_ in Fig. 392. _Cetus_,
the _Whale_, or the _Sea Monster_, shown in Fig. 393, belongs to the
same mythological group of constellations.

[Illustration: Fig. 394.]

339. _Scorpio, Sagittarius, and Ophiuchus._--During the summer months a
brilliant constellation is visible, called _Scorpio_, or the _Scorpion_.
The configuration of the chief stars of this constellation is shown in
Fig. 394. They bear some resemblance to a boy's kite. The brightest star
is of the first magnitude, and called _Antares_ (from _anti_, instead
of, and _Ares_, the Greek name of Mars), because it rivals Mars in
redness. The stars in the tail of the Scorpion are visible in our
latitude only under very favorable circumstances. This constellation is
shown in Fig. 395, together with _Sagittarius_ and _Ophiuchus_.
_Sagittarius_, or the _Archer_, is to the east of _Scorpio_. It contains
no bright stars, but is easily recognized from the fact that five of its
principal stars form the outline of an inverted dipper, which, from the
fact of its being partly in the Milky-Way, is often called the _Milk
Dipper_.

[Illustration: Fig. 395.]

_Ophiuchus_, or the _Serpent-Bearer_, is a large constellation, filling
all the space between the head of _Hercules_ and _Scorpio_. It is
difficult to trace, since it contains no very brilliant stars. This
constellation and _Libra_, or the _Balances_, which is the zodiacal
constellation to the west of Scorpio, are shown in Fig. 396.

[Illustration: Fig. 396.]

[Illustration: Fig. 397.]

340. _Capricornus, Aquarius, and the Southern Fish._--The two zodiacal
constellations to the east of Sagittarius are _Capricornus_ and
_Aquarius_. _Capricornus_ contains three pairs of small stars, which
mark the head, the tail, and the knees of the animal.

_Aquarius_ is marked by no conspicuous stars. An irregular line of
minute stars marks the course of the stream of water which flows from
the Water-Bearer's Urn into the mouth of the _Southern Fish_. This mouth
is marked by the first-magnitude star _Fomalhaut_. These constellations
are shown in Fig. 397.

[Illustration: Fig. 398.]

341. _Pisces and Aries._--The remaining zodiacal constellations are
_Pisces_, or the _Fishes_, _Aries_, or the _Ram_ (Fig. 398), and
_Cancer_, or the _Crab_.

The _Fishes_ lie under _Pegasus_ and _Andromeda_, but contain no bright
stars. _Aries_ (between _Pisces_ and _Taurus_) is marked by a pair of
stars on the head,--one of the second, and one of the third magnitude.
_Cancer_ (between _Leo_ and _Gemini_) has no bright stars, but contains
a remarkable cluster of small stars called _Præsepe_, or the _Beehive_.


                               Clusters.


342. _The Hyades._--The _Hyades_ are a very open cluster in the face of
_Taurus_ (334). The three brightest stars of this cluster form a letter
_V_, the point of the _V_ being on the nose, and the open ends at the
eyes. This cluster is shown in Fig. 399. The name, according to the most
probable etymology, means _rainy_; and they are said to have been so
called because their rising was associated with wet weather. They were
usually considered the daughters of Atlas, and sisters of the Pleiades,
though sometimes referred to as the nurses of Bacchus.

[Illustration: Fig. 399.]

343. _The Pleiades._--The _Pleiades_ constitute a celebrated group of
stars, or a miniature constellation, on the shoulder of _Taurus_. Hesiod
mentions them as "the seven virgins of Atlas born," and Milton calls
them "the seven Atlantic sisters." They are referred to in the Book of
Job. The Spaniards term them "the little nanny-goats;" and they are
sometimes called "the hen and chickens."

[Illustration: Fig. 400.]

[Illustration: Fig. 401.]

Usually only six stars in this cluster can be seen with the naked eye,
and this fact has given rise to the legend of the "lost Pleiad." On a
clear, moonless night, however, a good eye can discern seven or eight
stars, and some observers have distinguished as many as eleven. Fig. 400
shows the _Pleiades_ as they appear to the naked eye under the most
favorable circumstances. Fig. 401 shows this cluster as it appears in a
powerful telescope. With such an instrument more than five hundred stars
are visible.

344. _Cluster in the Sword-handle of Perseus._--This is a somewhat dense
double cluster. It is visible to the naked eye, appearing as a hazy
star. A line drawn from _Algenib_, or _Alpha_ of _Perseus_ (338), to
_Delta_ of _Cassiopeia_ (330), will pass through this cluster at about
two-thirds the distance from the former. This double cluster is one of
the most brilliant objects in the heavens, with a telescope of moderate
power.

[Illustration: Fig. 402.]

345. _Cluster of Hercules._--The celebrated globular cluster of
_Hercules_ can be seen only with a telescope of considerable power, and
to resolve it into distinct stars (as shown in Fig. 402) requires an
instrument of the very highest class.

[Illustration: Fig. 403.]

346. _Other Clusters._--Fig. 403 shows a magnificent globular cluster in
the constellation _Aquarius_. Herschel describes it as appearing like a
heap of sand, being composed of thousands of stars of the fifteenth
magnitude.

[Illustration: Fig. 404.]

Fig. 404 shows a cluster in the constellation _Toucan_, which Sir John
Herschel describes as a most glorious globular cluster, the stars of the
fourteenth magnitude being immensely numerous. There is a marked
condensation of light at the centre.

[Illustration: Fig. 405.]

[Illustration: Fig. 406.]

Fig. 405 shows a cluster in the _Centaur_, which, according to the same
astronomer, is beyond comparison the richest and largest object of the
kind in the heavens, the stars in it being literally innumerable. Fig.
406 shows a cluster in _Scorpio_, remarkable for the peculiar
arrangement of its component stars.

Star clusters are especially abundant in the region of the Milky-Way,
the law of their distribution being the reverse of that of the nebulæ.


                       Double and Multiple Stars.


347. _Double Stars._--The telescope shows that many stars which appear
single to the naked eye are really _double_, or composed of a pair of
stars lying side by side. There are several pairs of stars in the
heavens which lie so near together that they almost seem to touch when
seen with the naked eye.

[Illustration: Fig. 407.]

[Illustration: Fig. 408.]

Pairs of stars are not considered double unless the components are so
near together that they both appear in the field of view when examined
with a telescope. In the majority of the pairs classed as double stars
the distance between the components ranges from half a second to fifteen
seconds.

[Illustration: Fig. 409.]

_Epsilon Lyræ_ is a good example of a pair of stars that can barely be
separated with a good eye. Figs. 407 and 408 show this pair as it
appears in telescopes magnifying respectively four and fifteen times;
and Fig. 409 shows it as seen in a more powerful telescope, in which
each of the two components of the pair is seen to be a truly double
star.

[Illustration: Fig. 410.]

[Illustration: Fig. 411.]

348. _Multiple Stars._--When a star is resolved into more than two
components by a telescope, it is called a _multiple_ star. Fig. 410
shows a _triple_ star in _Pegasus_. Fig. 411 shows a quadruple star in
_Taurus_. Fig. 412 shows a _sextuple_ star, and Fig. 413 a _septuple_
star. Fig. 414 shows the celebrated septuple star in _Orion_, called
_Theta Orionis_, or the _trapezium_ of Orion.

349. _Optically Double and Multiple Stars._--Two or more stars which are
really very distant from each other, and which have no physical
connection whatever, may appear to be near together, because they happen
to lie in the same direction, one behind the other. Such accidental
combinations are called _optically_ double or multiple stars.

[Illustration: Fig. 412.]

[Illustration: Fig. 413.]

350. _Physically Double and Multiple Stars._--In the majority of cases
the components of double and multiple stars are in reality comparatively
near together, and are bound together by gravity into a physical system.
Such combinations are called _physically_ double and multiple stars. The
components of these systems all revolve around their common centre of
gravity. In many instances their orbits and periods of revolution have
been ascertained by observation and calculation. Fig. 415 shows the
orbit of one of the components of a double star in the constellation
_Hercules_.

[Illustration: Fig. 414.]

351. _Colors of Double and Multiple Stars._--The components of double
and multiple stars are often highly colored, and frequently the
components of the same system are of different colors. Sometimes one
star of a binary system is _white_, and the other _red_; and sometimes a
_white_ star is combined with a _blue_ one. Other colors found in
combination in these systems are _red_ and _blue_, _orange_ and _green_,
_blue_ and _green_, _yellow_ and _blue_, _yellow_ and _red_, etc.

[Illustration: Fig. 415.]

If these double and multiple stars are accompanied by planets, these
planets will sometimes have two or more suns in the sky at once. On
alternate days they may have suns of different colors, and perhaps on
the same day two suns of different colors. The effect of these changing
colored lights on the landscape must be very remarkable.


                        New and Variable Stars.


352. _Variable Stars._--There are many stars which undergo changes of
brilliancy, sometimes slight, but occasionally very marked. These
changes are in some cases apparently irregular, and in others
_periodic_. All such stars are said to be _variable_, though the term is
applied especially to those stars whose variability is _periodic_.

[Illustration: Fig. 416.]

353. _Algol._--_Algol_, a star of _Perseus_, whose position is shown in
Fig. 416, is a remarkable variable star of a short period. Usually it
shines as a faint second-magnitude star; but at intervals of a little
less than three days it fades to the fourth magnitude for a few hours,
and then regains its former brightness. These changes were first noticed
some two centuries ago, but it was not till 1782 that they were
accurately observed. The period is now known to be two days, twenty
hours, forty-nine minutes. It takes about four hours and a half to fade
away, and four hours more to recover its brilliancy. Near the beginning
and end of the variations, the change is very slow, so that there are
not more than five or six hours during which an ordinary observer would
see that the star was less bright than usual.

This variation of light was at first explained by supposing that a large
dark planet was revolving round Algol, and passed over its face at every
revolution, thus cutting off a portion of its light; but there are small
irregularities in the variation, which this theory does not account for.

354. _Mira._--Another remarkable variable star is _Omicron Ceti_, or
_Mira_ (that is, the _wonderful_ star). It is generally invisible to the
naked eye; but at intervals of about eleven months it shines forth as a
star of the second or third magnitude. It is about forty days from the
time it becomes visible until it attains its greatest brightness, and is
then about two months in fading to invisibility; so that its increase of
brilliancy is more rapid than its waning. Its period is quite irregular,
ranging from ten to twelve months; so that the times of its appearance
cannot be predicted with certainty. Its maximum brightness is also
variable, being sometimes of the second magnitude, and at others only of
the third or fourth.

[Illustration: Fig. 417.]

355. _Eta Argus._--Perhaps the most extraordinary variable star in the
heavens is _Eta Argus_, in the constellation _Argo_, or the _Ship_, in
the southern hemisphere (Fig. 417). The first careful observations of
its variability were made by Sir John Herschel while at the Cape of Good
Hope. He says, "It was on the 16th of December, 1837, that, resuming the
photometrical comparisons, my astonishment was excited by the appearance
of a new candidate for distinction among the very brightest stars of the
first magnitude in a part of the heavens where, being perfectly familiar
with it, I was certain that no such brilliant object had before been
seen. After a momentary hesitation, the natural consequence of a
phenomenon so utterly unexpected, and referring to a map for its
configuration with other conspicuous stars in the neighborhood, I became
satisfied of its identity with my old acquaintance, _Eta Argus_. Its
light was, however, nearly tripled. While yet low, it equalled Rigel,
and, when it attained some altitude, was decidedly greater." It
continued to increase until Jan. 2, 1838, then faded a little till April
following, though it was still as bright as Aldebaran. In 1842 and 1843
it blazed up brighter than ever, and in March of the latter year was
second only to _Sirius_. During the twenty-five years following it
slowly but steadily diminished. In 1867 it was barely visible to the
naked eye; and the next year it vanished entirely from the unassisted
view, and has not yet begun to recover its brightness. The curve in Fig.
418 shows the change in brightness of this remarkable star. The numbers
at the bottom show the years of the century, and those at the side the
brightness of the star.

[Illustration: Fig. 418.]

356. _New Stars._--In several cases stars have suddenly appeared, and
even become very brilliant; then, after a longer or shorter time, they
have faded away and disappeared. Such stars are called _new_ or
_temporary_ stars. For a time it was supposed that such stars were
actually new. They are now, however, classified by astronomers among the
variable stars, their changes being of a very irregular and fitful
character. There is scarcely a doubt that they were all in the heavens
as very small stars before they blazed forth in so extraordinary a
manner, and that they are in the same places still. There is a wide
difference between these irregular variations, or the breaking-forth of
light on a single occasion in the course of centuries, and the regular
and periodic changes in the case of a star like _Algol_; but a long
series of careful observation has resulted in the discovery of stars of
nearly every degree of irregularity between these two extremes. Some of
them change gradually from one magnitude to another, in the course of
years, without seeming to follow any law whatever; while in others some
slight tendency to regularity can be traced. _Eta Argus_ may be regarded
as a connecting link between new and variable stars.

357. _Tycho Brahe's Star._--An apparently new star suddenly appeared in
_Cassiopeia_ in 1572. It was first seen by Tycho Brahe, and is therefore
associated with his name. Its position in the constellation is shown in
Fig. 419. It was first seen on Nov. 11, when it had already attained the
first magnitude. It became rapidly brighter, soon rivalling Venus in
splendor, so that good eyes could discern it in full daylight. In
December it began to wane, and gradually faded until the following May,
when it disappeared entirely.

[Illustration: Fig. 419.]

A star showed itself in the same part of the heavens in 945 and in 1264.
If these were three appearances of the same star, it must be reckoned as
a periodic star with a period of a little more than three hundred years.

358. _Kepler's Star._--In 1604 a new star was seen in the constellation
_Ophiuchus_. It was first noticed in October of that year, when it was
of the first magnitude. In the following winter it began to fade, but
remained visible during the whole year 1605. Early in 1606 it
disappeared entirely. A very full history of this star was written by
Kepler.

One of the most remarkable things about this star was its brilliant
scintillation. According to Kepler, it displayed all the colors of the
rainbow, or of a diamond cut with multiple facets, and exposed to the
rays of the sun. It is thought that this star also appeared in 393, 798,
and 1203; if so, it is a variable star with a period of a little over
four hundred years.

359. _New Star of 1866._--The most striking case of this kind in recent
times was in May, 1866, when a star of the second magnitude suddenly
appeared in _Corona Borealis_. On the 11th and 12th of that month it was
observed independently by at least five observers in Europe and America.
The fact that none of these new stars were noticed until they had nearly
or quite attained their greatest brilliancy renders it probable that
they all blazed up very suddenly.

360. _Cause of the Variability of Stars._--The changes in the brightness
of variable and temporary stars are probably due to operations similar
to those which produce the spots and prominences in our sun. We have
seen (188) that the frequency of solar spots shows a period of eleven
years, during one portion of which there are few or no spots to be seen,
while during another portion they are numerous. If an observer so far
away as to see our sun like a star could from time to time measure its
light exactly, he would find it to be a variable star with a period of
eleven years, the light being least when we see most spots, and greatest
when few are visible. The variation would be slight, but it would
nevertheless exist. Now, we have reason to believe that the physical
constitution of the sun and the stars is of the same general nature. It
is therefore probable, that, if we could get a nearer view of the stars,
we should see spots on their disks as we do on the sun. It is also
likely that the varying physical constitution of the stars might give
rise to great differences in the number and size of the spots; so that
the light of some of these suns might vary to a far greater degree than
that of our own sun does. If the variations had a regular period, as in
the case of our sun, the appearances to a distant observer would be
precisely what we see in the case of a periodic variable star.

The spectrum of the new star of 1866 was found to be a continuous one,
crossed by bright lines, which were apparently due to glowing hydrogen.
The continuous spectrum was also crossed by dark lines, indicating that
the light had passed through an atmosphere of comparatively cool gas.
Mr. Huggins infers from this that there was a sudden and extraordinary
outburst of hydrogen gas from the star, which by its own light, as well
as by heating up the whole surface of the star, caused the extraordinary
increase of brilliancy. Now, the spectroscope shows that the red flames
of the solar chromosphere (197) are largely composed of hydrogen; and it
is not unlikely that the blazing-forth of this star arose from an action
similar to that which produces these flames, only on an immensely larger
scale.


                         Distance of the Stars.


361. _Parallax of the Stars._--Such is the distance of the stars, that
only in a comparatively few instances has any displacement of these
bodies been detected when viewed from opposite parts of the earth's
orbit, that is, from points a hundred and eighty-five million miles
apart; and in no case can this displacement be detected except by the
most careful and delicate measurement. Half of the above displacement,
or the displacement of the star as seen from the earth instead of the
sun, is called the _parallax_ of the star. In no case has a parallax of
one second as yet been detected.

362. _The Distance of the Stars._--The distance of a star whose parallax
is one second would be 206,265 times the distance of the earth from the
sun, or about nineteen million million miles. It is quite certain that
no star is nearer than this to the earth. Light has a velocity which
would carry it seven times and a half around the earth in a second; but
it would take it more than three years to reach us from that distance.
Were all the stars blotted out of existence to-night, it would be at
least three years before we should miss a single one.

_Alpha Centauri_, the brightest star in the constellation of the
_Centaur_, is, so far as we know, the nearest of the fixed stars. It is
estimated that it would take its light about three years and a half to
reach us. It has also been estimated that it would take light over
sixteen years to reach us from _Sirius_, about eighteen years to reach
us from _Vega_, about twenty-five years from _Arcturus_, and over forty
years from the _Pole-Star_. In many instances it is believed that it
would take the light of stars hundreds of years to make the journey to
our earth, and in some instances even thousands of years.


                      Proper Motion of the Stars.


363. _Why the Stars appear Fixed._--The stars seem to retain their
relative positions in the heavens from year to year, and from age to
age; and hence they have come universally to be denominated as _fixed_.
It is, however, now well known that the stars, instead of being really
stationary, are moving at the rate of many miles a second; but their
distance is so enormous, that, in the majority of cases, it would be
thousands of years before this rate of motion would produce a sufficient
displacement to be noticeable to the unaided eye.

[Illustration: Fig. 420.]

364. _Secular Displacement of the Stars._--Though the proper motion of
the stars is apparently slight, it will, in the course of many ages,
produce a marked change in the configuration of the stars. Thus, in Fig.
420, the left-hand portion shows the present configuration of the stars
of the Great Dipper. The small arrows attached to the stars show the
direction and comparative magnitudes of their motion. The right-hand
portion of the figure shows these stars as they will appear thirty-six
thousand years from the present time.

[Illustration: Fig. 421.]

Fig. 421 shows in a similar way the present configuration and proper
motion of the stars of _Cassiopeia_, and also these stars as they will
appear thirty-six thousand years hence.

[Illustration: Fig. 422.]

Fig. 422 shows the same for the constellation _Orion_.

365. _The Secular Motion of the Sun._--The stars in all parts of the
heavens are found to move in all directions and with all sorts of
velocities. When, however, the motions of the stars are averaged, there
is found to be an apparent proper motion common to all the stars. The
stars in the neighborhood of _Hercules_ appear to be approaching us, and
those in the opposite part of the heavens appear to be receding from us.
In other words, all the stars appear to be moving away from Hercules,
and towards the opposite part of the heavens.

[Illustration: Fig. 423.]

This apparent motion common to all the stars is held by astronomers to
be due to the real motion of the sun through space. The point in the
heavens towards which our sun is moving at the present time is indicated
by the small circle in the constellation Hercules in Fig. 423. As the
sun moves, he carries the earth and all the planets along with him. Fig.
424 shows the direction of the sun's motion with reference to the
ecliptic and to the axis of the earth. Fig. 425 shows the earth's path
in space; and Fig. 426 shows the paths of the earth, the moon, Mercury,
Venus, and Mars in space.

[Illustration: Fig. 424.]

[Illustration: Fig. 425.]

[Illustration: Fig. 426.]

Whether the sun is actually moving in a straight line, or around some
distant centre, it is impossible to determine at the present time. It is
estimated that the sun is moving along his path at the rate of about a
hundred and fifty million miles a year. This is about five-sixths of the
diameter of the earth's orbit.

366. _Star-Drift._--In several instances, groups of stars have a common
proper motion entirely different from that of the stars around and among
them. Such groups probably form connected systems, in the motion of
which all the stars are carried along together without any great change
in their relative positions. The most remarkable case of this kind
occurs in the constellation _Taurus_. A large majority of the brighter
stars in the region between _Aldebaran_ and the _Pleiades_ have a common
proper motion of about ten seconds per century towards the east. Proctor
has shown that five out of the seven stars which form the Great Dipper
have a common proper motion, as shown in Fig. 427 (see also Fig. 420).
He proposes for this phenomenon the name of _Star-Drift_.

[Illustration: Fig. 427.]

367. _Motion of Stars along the Line of Sight._--A motion of a star in
the direction of the line of sight would produce no displacement of the
star that could be detected with the telescope; but it would cause a
change in the brightness of the star, which would become gradually
fainter if moving from us, and brighter if approaching us. Motion along
the line of sight has, however, been detected by the use of the
tele-spectroscope (152), owing to the fact that it causes a displacement
of the spectral lines. As has already been explained (169), a
displacement of a spectral line towards the red end of the spectrum
indicates a motion away from us, and a displacement towards the violet
end, a motion towards us.

                  *       *       *       *       *

By means of these displacements of the spectral lines, Huggins has
detected motion in the case of a large number of stars, and calculated
its rate:--

STARS RECEDING FROM US.

    Sirius                  20 miles per second.
    Betelgeuse              22 miles per second.
    Rigel                   15 miles per second.
    Castor                  25 miles per second.
    Regulus                 15 miles per second.

STARS APPROACHING US.

    Arcturus                55 miles per second.
    Vega                    50 miles per second.
    Deneb                   39 miles per second.
    Pollux                  49 miles per second.
    Alpha Ursæ Majoris      46 miles per second.

These results are confirmed by the fact that the amount of motion
indicated is about what we should expect the stars to have, from their
observed proper motions, combined with their probable distances. Again:
the stars in the neighborhood of Hercules are mostly found to be
approaching the earth, and those which lie in the opposite direction to
be receding from it; which is exactly the effect which would result from
the sun's motion through space. The five stars in the Dipper, which have
a common proper motion, are also found to have a common motion in the
line of sight. But the displacement of the spectral lines is so slight,
and its measurement so difficult, that the velocities in the above table
are to be accepted as only an approximation to the true values.


            Chemical and Physical Constitution of the Stars.


368. _The Constitution of the Stars Similar to that of the Sun._--The
stellar spectra bear a general resemblance to that of the sun, with
characteristic differences. These spectra all show Fraunhofer's lines,
which indicate that their luminous surfaces are surrounded by
atmospheres containing absorbent vapors, as in the case of the sun. The
positions of these lines indicate that the stellar atmospheres contain
elements which are also found in the sun's, and on the earth.

[Illustration: Fig. 428.]

369. _Four Types of Stellar Spectra._--The spectra of the stars have
been carefully observed by Secchi and Huggins. They have found that
stellar spectra may be reduced to four types, which are shown in Fig.
428. In the spectrum of _Sirius_, a representative of _Type I._, very
few lines are represented; but the lines are very thick.

Next we have the solar spectrum, which is a representative of _Type
II._, one in which more lines are represented. In _Type III._ fluted
spaces begin to appear, and in _Type IV._, which is that of the red
stars, nothing but fluted spaces is visible; and this spectrum shows
that something is at work in the atmosphere of those red stars different
from what there is in the simpler atmosphere of _Type I._

Lockyer holds that these differences of spectra are due simply to
differences of temperature. According to him, the red stars, which give
the fluted spectra, are of the lowest temperature; and the temperature
of the stars of the different types gradually rises till we reach the
first type, in which the temperature is so high that the dissociation
(161) of the elements is nearly if not quite complete.




                              III. NEBULÆ.


                       Classification of Nebulæ.


370. _Planetary Nebulæ._--Many nebulæ (328) present a well-defined
circular disk, like that of a planet, and are therefore called
_planetary_ nebulæ. Specimens of planetary nebulæ are shown in Fig. 429.

[Illustration: Fig. 429.]

371. _Circular and Elliptical Nebulæ._--While many nebulæ are circular
in form, others are elliptical. The former are called _circular_ nebulæ,
and the latter _elliptical_ nebulæ. Elliptical nebulæ have been
discovered of every degree of eccentricity. Examples of various circular
and elliptical nebulæ are given in Fig. 430.

[Illustration: Fig. 430.]

372. _Annular Nebulæ._--Occasionally ring-shaped nebulæ have been
observed, sometimes with, and sometimes without, nebulous matter within
the ring. They are called _annular_ nebulæ. They are both circular and
elliptical in form. Several specimens of this class of nebulæ are given
in Fig. 431.

[Illustration: Fig. 431.]

373. _Nebulous Stars._--Sometimes one or more minute stars are enveloped
in a nebulous haze, and are hence called _nebulous stars_. Several of
these nebulæ are shown in Fig. 432.

[Illustration: Fig. 432.]

374. _Spiral Nebulæ._--Very many nebulæ disclose a more or less spiral
structure, and are known as _spiral_ nebulæ. They are illustrated in
Fig. 433. There are, however, a great variety of spiral forms. We shall
have occasion to speak of these nebulæ again (381-383).

[Illustration: Fig. 433.]

375. _Double and Multiple Nebulæ._--Many _double_ and _multiple_ nebulæ
have been observed, some of which are represented in Fig. 434.

[Illustration: Fig. 434.]

Fig. 435 shows what appears to be a double annular nebula. Fig. 436
gives two views of a double nebula. The change of position in the
components of this double nebula indicates a motion of revolution
similar to that of the components of double stars.

[Illustration: Fig. 435.]

[Illustration: Fig. 436.]


                           Irregular Nebulæ.


376. _Irregular Forms._--Besides the more or less regular forms of
nebulæ which have been classified as indicated above, there are many of
very irregular shapes, and some of these are the most remarkable nebulæ
in the heavens. Fig. 437 shows a curiously shaped nebula, seen by Sir
John Herschel in the southern heavens; and Fig. 438, one in _Taurus_,
known as the _Crab_ nebula.

[Illustration: Fig. 437.]

[Illustration: Fig. 438.]

377. _The Great Nebula of Andromeda._--This is one of the few nebulæ
that are visible to the naked eye. We see at a glance that it is not a
star, but a mass of diffused light. Indeed, it has sometimes been very
naturally mistaken for a comet. It was first described by Marius in
1614, who compared its light to that of a candle shining through horn.
This gives a very good idea of the impression it produces, which is that
of a translucent object illuminated by a brilliant light behind it. With
a small telescope it is easy to imagine it to be a solid like horn; but
with a large one the effect is more like fog or mist with a bright body
in its midst. Unlike most of the nebulæ, its spectrum is a continuous
one, similar to that from a heated solid, indicating that the light
emanates, not from a glowing gas, but from matter in the solid or liquid
state. This would suggest that it is really an immense star-cluster, so
distant that the highest telescopic power cannot resolve it; yet in the
largest telescopes it looks less resolvable, and more like a gas, than
in those of moderate size. If it is really a gas, and if the spectrum is
continuous throughout the whole extent of the nebula, either it must
shine by reflected light, or the gas must be subjected to a great
pressure almost to its outer limit, which is hardly possible. If the
light is reflected, we cannot determine whether it comes from a single
bright star, or a number of small ones scattered through the nebula.

With a small telescope this nebula appears elliptical, as in Fig. 439.
Fig. 440 shows it as it appeared to Bond, in the Cambridge refractor.

[Illustration: Fig. 439.]

[Illustration: Fig. 440.]

378. _The Great Nebula of Orion._--The nebula which, above all others,
has occupied the attention of astronomers, and excited the wonder of
observers, is the _great nebula of Orion_, which surrounds the middle
star of the three which form the sword of Orion. A good eye will
perceive that this star, instead of looking like a bright point, has a
hazy appearance, due to the surrounding nebula. This object was first
described by Huyghens in 1659, as follows:--

"There is one phenomenon among the fixed stars worthy of mention, which,
so far as I know, has hitherto been noticed by no one, and indeed cannot
be well observed except with large telescopes. In the sword of Orion are
three stars quite close together. In 1656, as I chanced to be viewing
the middle one of these with the telescope, instead of a single star,
twelve showed themselves (a not uncommon circumstance). Three of these
almost touched each other, and with four others shone through a nebula,
so that the space around them seemed far brighter than the rest of the
heavens, which was entirely clear, and appeared quite black; the effect
being that of an opening in the sky, through which a brighter region was
visible."

[Illustration: Fig. 441.]

The representation of this nebula in Fig. 441 is from a drawing made by
Bond. In brilliancy and variety of detail it exceeds any other nebula
visible in the northern hemisphere. In its centre are four stars, easily
distinguished by a small telescope with a magnifying power of forty or
fifty, together with two smaller ones, requiring a nine-inch telescope
to be well seen. Besides these, the whole nebula is dotted with stars.

In the winter of 1864-65 the spectrum of this nebula was examined
independently by Secchi and Huggins, who found that it consisted of
three bright lines, and hence concluded that the nebula was composed,
not of stars, but of glowing gas. The position of one of the lines was
near that of a line of nitrogen, while another seemed to coincide with a
hydrogen line. This would suggest that the nebula is a mixture of
hydrogen and nitrogen gas; but of this we cannot be certain.

[Illustration: Fig. 442.]

379. _The Nebula in Argus._--There is a nebula (Fig. 442) surrounding
the variable star _Eta Argus_ (355), which is remarkable as exhibiting
variations of brightness and of outline.

In many other nebulæ, changes have been suspected; but the
indistinctness of outline which characterizes most of these objects, and
the very different aspect they present in telescopes of different
powers, render it difficult to prove a change beyond a doubt.

380. _The Dumb-Bell Nebula._--This nebula was named from its peculiar
shape. It is a good illustration of the change in the appearance of a
nebula when viewed with different magnifying powers. Fig. 443 shows it
as it appeared in Herschel's telescope, and Fig. 444 as it appears in
the great Parsonstown reflector (20).

[Illustration: Fig. 443.]

[Illustration: Fig. 444.]


                             Spiral Nebulæ.


381. _The Spiral Nebula in Canes Venatici._--The great spiral nebula in
the constellation _Canes Venatici_, or the _Hunting-Dogs_, is one of the
most remarkable of its class. Fig. 445 shows this nebula as it appeared
in Herschel's telescope, and Fig. 446 shows it as it appears in the
Parsonstown reflector.

[Illustration: Fig. 445.]

[Illustration: Fig. 446.]

382. _Condensation of Nebulæ._--The appearance of the nebula just
mentioned suggests a body rotating on its axis, and undergoing
condensation at the same time.

It is now a generally received theory that nebulæ are the material out
of which stars are formed. According to this theory, the stars
originally existed as nebulæ, and all nebulæ will ultimately become
condensed into stars.

[Illustration: Fig. 447.]

[Illustration: Fig. 448.]

[Illustration: Fig. 449.]

383. _Other Spiral Nebulæ._--Fig. 447 represents a spiral nebula of the
_Great Bear_. This nebula seems to have several centres of condensation.
Fig. 448 is a view of a spiral nebula in _Cepheus_, and Fig. 449 of a
singular spiral nebula in the _Triangle_. This also appears to have
several points of condensation. Figs. 450 and 451 represent oval and
elliptical nebulæ having a spiral structure.

[Illustration: Fig. 450.]

[Illustration: Fig. 451.]

_THE MAGELLANIC CLOUDS._

[Illustration: Fig. 452.]

384. _Situation and General Appearance of the Magellanic Clouds._--The
_Magellanic clouds_ are two nebulous-looking bodies near the southern
pole of the heavens, as shown in the right-hand portion of Fig. 452. In
the appearance and brightness of their light they resemble portions of
the Milky-Way.

[Illustration: Fig. 453.]

The larger of these clouds is called the _Nubecula Major_. It is visible
to the naked eye in strong moonlight, and covers a space about two
hundred times the surface of the moon. It is shown in Fig. 453. The
smaller cloud is called the _Nubecula Minor_. It has only about a fourth
the extent of the larger cloud, and is considerably less brilliant. It
is visible to the naked eye, but it disappears in full moonlight. This
cloud is shown in Fig. 454. The region around this cloud is singularly
bare of stars; but the magnificent cluster of _Toucan_, already
described (346), is near, and is shown a little to the right of the
cloud in the figure.

[Illustration: Fig. 454.]

[Illustration: Fig. 455.]

385. _Structure of the Nubeculæ._--Fig. 455 shows the structure of these
clouds as revealed by a powerful telescope. The general ground of both
consists of large tracts and patches of nebulosity in every stage of
resolution,--from that which is irresolvable with eighteen inches of
reflecting aperture, up to perfectly separated stars, like the Milky-Way
and clustering groups. There are also nebulæ in abundance, both regular
and irregular, globular clusters in every state of condensation, and
objects of a nebulous character quite peculiar, and unlike any thing in
other regions of the heavens. In the area occupied by the _nubecula
major_ two hundred and seventy-eight nebulæ and clusters have been
enumerated, besides fifty or sixty outliers, which ought certainly to be
reckoned as its appendages, being about six and a half per square
degree; which very far exceeds the average of any other part of the
nebulous heavens. In the _nubecula minor_ the concentration of such
objects is less, though still very striking. The nubeculæ, then,
combine, each within its own area, characters which in the rest of the
heavens are no less strikingly separated; namely, those of the galactic
and the nebular system. Globular clusters (except in one region of small
extent) and nebulæ of regular elliptic forms are comparatively rare in
the Milky-Way, and are found congregated in the greatest abundance in a
part of the heavens the most remote possible from that circle; whereas
in the nubeculæ they are indiscriminately mixed with the general starry
ground, and with irregular though small nebulæ.


                        THE NEBULAR HYPOTHESIS.


    386. _The Basis of the Nebular Hypothesis._--We have seen that the
    planets all revolve around the sun from west to east in nearly the
    same plane, and that the sun rotates on his axis from west to east.
    The planets, so far as known, rotate on their axes from west to
    east; and all the moons, except those of Uranus and Neptune, revolve
    around their planets from west to east. These common features in the
    motion of the sun, moons, and planets, point to the conclusion that
    they are of a common origin.

    387. _Kant's Hypothesis._--Kant, the celebrated German philosopher,
    seems to have the best right to be regarded as the founder of the
    modern nebular hypothesis. His reasoning has been concisely stated
    thus: "Examining the solar system, we find two remarkable features
    presented to our consideration. One is, that six planets and nine
    satellites [the entire number then known] move around the sun in
    circles, not only in the same direction in which the sun himself
    revolves on his axis, but very nearly in the same plane. This common
    feature of the motion of so many bodies could not by any reasonable
    possibility have been a result of chance: we are therefore forced to
    believe that it must be the result of some common cause originally
    acting on all the planets.

    "On the other hand, when we consider the spaces in which the planets
    move, we find them entirely void, or as good as void; for, if there
    is any matter in them, it is so rare as to be without effect on the
    planetary motions. There is, therefore, no material connection now
    existing between the planets through which they might have been
    forced to take up a common direction of motion. How, then, are we to
    reconcile this common motion with the absence of all material
    connection? The most natural way is to suppose that there was once
    some such connection, which brought about the uniformity of motion
    which we observe; that the materials of which the planets are formed
    once filled the whole space between them. There was no formation in
    this chaos, the formation of separate bodies by the mutual
    gravitation of parts of the mass being a later occurrence. But,
    naturally, some parts of the mass would be more dense than others,
    and would thus gather around them the rare matter which filled the
    intervening spaces. The larger collections thus formed would draw
    the smaller ones into them, and this process would continue until a
    few round bodies had taken the place of the original chaotic mass."

    Kant, however, failed to account satisfactorily for the motion of
    the sun and planets. According to his system, all the bodies formed
    out of the original nebulous mass should have been drawn to a common
    centre so as to form one sun, instead of a system of revolving
    bodies like the solar system.

    388. _Herschel's Hypothesis._--The idea of the gradual transmutation
    of nebulæ into stars seems to have been suggested to Herschel, not
    by the study of the solar system, but by that of the nebulæ
    themselves. Many of these bodies he believed to be immense masses of
    phosphorescent vapor; and he conceived that these must be gradually
    condensing, each around its own centre, or around the parts where it
    is most dense, until it should become a star, or a cluster of stars.
    On classifying the nebulæ, it seemed to him that he could see this
    process going on before his eyes. There were the large, faint,
    diffused nebulæ, in which the condensation had hardly begun; the
    smaller but brighter ones, which had become so far condensed that
    the central parts would soon begin to form into stars; yet others,
    in which stars had actually begun to form; and, finally,
    star-clusters in which the condensation was complete. The
    spectroscopic revelations of the gaseous nature of the true nebulæ
    tend to confirm the theory of Herschel, that these masses will all,
    at some time, condense into stars.

    389. _Laplace's Hypothesis._--Laplace was led to the nebular
    hypothesis by considering the remarkable uniformity in the direction
    of the rotation of the planets. Believing that this could not have
    been the result of chance, he sought to investigate its cause. This,
    he thought, could be nothing else than the atmosphere of the sun,
    which once extended so far out as to fill all the space now occupied
    by the planets. He begins with the sun, surrounded by this immense
    fiery atmosphere. Since the sum total of rotary motion now seen in
    the planetary system must have been there from the beginning, he
    conceives the immense vaporous mass forming the sun and his
    atmosphere to have had a slow rotation on its axis. As the intensely
    hot mass gradually cooled, it would contract towards the centre. As
    it contracted, its velocity of rotation would, by the laws of
    mechanics, constantly increase; so that a time would arrive, when,
    at the outer boundary of the mass, the centrifugal force due to the
    rotation would counterbalance the attractive force of the central
    mass. Then those outer portions would be left behind as a revolving
    ring, while the next inner portions would continue to contract until
    the centrifugal and attractive forces were again balanced, when a
    second ring would be left behind; and so on. Thus, instead of a
    continuous atmosphere, the sun would be surrounded by a series of
    concentric revolving rings of vapor. As these rings cooled, their
    denser materials would condense first; and thus the ring would be
    composed of a mixed mass, partly solid and partly vaporous, the
    quantity of solid matter constantly increasing, and that of vapor
    diminishing. If the ring were perfectly uniform, this condensation
    would take place equally all around it, and the ring would thus be
    broken up into a group of small planets, like the asteroids. But if,
    as would more likely be the case, some portions of the ring were
    much denser than others, the denser portions would gradually attract
    the rarer portions, until, instead of a ring, there would be a
    single mass composed of a nearly solid centre, surrounded by an
    immense atmosphere of fiery vapor. This condensation of the ring of
    vapor around a single point would not change the amount of rotary
    motion that had existed in the ring. The planet with its atmosphere
    would therefore be in rotation; and would be, on a smaller scale,
    like the original solar mass surrounded by its atmosphere. In the
    same way that the latter formed itself first into rings, which
    afterwards condensed into planets, so the planetary atmospheres, if
    sufficiently extensive, would form themselves into rings, which
    would condense into satellites. In the case of Saturn, however, one
    of the rings was so uniform throughout, that there was no denser
    portion to attract the rest around it; and thus the ring of Saturn
    retained its annular form.

    [Illustration: Fig. 456.]

    Such is the celebrated nebular hypothesis of Laplace. It starts, not
    with a purely nebulous mass, but with the sun, surrounded by an
    immense atmosphere, out of which the planets were formed by gradual
    condensation. Fig. 456 represents the condensing mass according to
    this theory.

    390. _The Modern Nebular Hypothesis._--According to the nebular
    hypothesis as held at the present time, the sun, planets, and
    meteoroids originated from a purely nebulous mass. This nebula first
    condensed into a nebulous star, the star being the sun, and its
    surrounding nebulosity being the fiery atmosphere of Laplace. The
    original nebula must have been put into rotation at the beginning.
    As it contracted and became condensed through the loss of heat by
    radiation into space, and under the combined attraction of gravity,
    cohesion, and affinity, its speed of rotation increased; and the
    nebulous envelop became, by the centrifugal force, flattened into a
    thin disk, which finally broke up into rings, out of which were
    formed the planets and their moons. According to Laplace, the rings
    which were condensed into the planets were thrown off in succession
    from the equatorial region of the condensing nebula; and so the
    outer planets would be the older. According to the more modern idea,
    the nebulous mass was first flattened into a disk, and subsequently
    broken up into rings, in such a way that there would be no marked
    difference in the ages of the planets. The sun represents the
    central portion of the original nebula, and the comets and
    meteoroids its outlying portion. At the sun the condensation is
    still going on, and the meteoroids appear to be still gradually
    drawn in to the sun and planets.

    The whole store of energy with which the original solar nebula was
    endowed existed in it in the potential form. By the condensation and
    contraction this energy was gradually transformed into the kinetic
    energy of molar motion and of heat; and the heat became gradually
    dissipated by radiation into space. This transformation of potential
    energy into heat is still going on at the sun, the centre of the
    condensing mass, by the condensation of the sun itself, and by the
    impact of meteors as they fall into it.

    It has been calculated, that, by the shrinking of the sun to the
    density of the earth, the transformation of potential energy into
    heat would generate enough heat to maintain the sun's supply, at the
    present rate of dissipation, for seventeen million years. A
    shrinkage of the sun which would generate all the heat he has poured
    into space since the invention of the telescope could not be
    detected by the most powerful instruments yet constructed.

    The least velocity with which a meteoroid could strike the sun would
    be two hundred and eighty miles a second; and it is easy to
    calculate how much heat would be generated by the collision. It has
    been shown, that, were enough meteoroids to fall into the sun to
    develop its heat, they would not increase his mass appreciably
    during a period of two thousand years.

    The sun's heat is undoubtedly developed by contraction and the fall
    of meteoroids; that is to say, by the transformation of the
    potential energy of the original nebula into heat.

    It must be borne in mind that the nebular hypothesis is simply a
    supposition as to the way in which the present solar system may have
    been developed from a nebula endowed with a motion of rotation and
    with certain tendencies to condensation. Of course nothing could
    have been developed out of the nebula, the germs of which had not
    been originally implanted in it by the Creator.


               IV. THE STRUCTURE OF THE STELLAR UNIVERSE.


391. _Sir William Herschel's View._--Sir William Herschel assumed that
the stars are distributed with tolerable uniformity throughout the space
occupied by our stellar system. He accounted for the increase in the
number of stars in the field of view as he approached the plane of the
Milky-Way, not by the supposition that the stars are really closer
together in and about this plane, but by the supposition that our
stellar system is in the form of a flat disk cloven at one side, and
with our sun near its centre. A section of this disk is shown in Fig.
457.

[Illustration: Fig. 457.]

An observer near _S_, with his telescope pointed in the direction of _S
b_, would see comparatively few stars within the field of view, because
looking through a comparatively thin stratum of stars. With his
telescope pointed in the direction _S a_, he would see many more stars
within his field of view, even though the stars were really no nearer
together, because he would be looking through a thicker stratum of
stars. As he directed his telescope more and more nearly in the
direction _S f_, he would be looking through a thicker and thicker
stratum of stars, and hence he would see a greater and greater number of
them in the field of view, though they were everywhere in the disk
distributed at uniform distances. He assumed, also, that the stars are
all tolerably uniform in size, and that certain stars appear smaller
than others, only because they are farther off. He supposed the faint
stars of the Milky-Way to be merely the most distant stars of the
stellar disk; that they are really as large as the other stars, but
appear small owing to their great distance. The disk was assumed to be
cloven on one side, to account for the division of the Milky-Way through
nearly half of its course. This theory of the structure of the stellar
universe is often referred to as the _cloven disk_ theory.

[Illustration: Fig. 458.]

392. _The Cloven Ring Theory._--According to Mädler, the stars of the
Milky-Way are entirely separated from the other stars of our system,
belonging to an outlying ring, or system of rings. To account for the
division of the Milky-Way, the ring is supposed to be cloven on one
side: hence this theory is often referred to as the _cloven ring_
theory. According to this hypothesis, the stellar system viewed from
without would present an appearance somewhat like that in Fig. 458. The
outlying ring cloven on one side would represent the stars of the
Milky-Way; and the luminous mass at the centre, the remaining stars of
the system.

393. _Proctor's View._--According to Proctor, the Milky-Way is composed
of an irregular spiral stream of minute stars lying in and among the
larger stars of our system, as represented in Fig. 459. The spiral
stream is shown in the inner circle as it really exists among the stars,
and in the outer circle as it is seen projected upon the sky. According
to this view, the stars of the Milky-Way appear faint, not because they
are distant, but because they are really small.

[Illustration: Fig. 459.]

394. _Newcomb's View._--According to Newcomb, the stars of our system
are all situated in a comparatively thin zone lying in the plane of the
Milky-Way, while there is a zone of nebulæ lying on each side of the
stellar zone. He believes that so much is certain with reference to the
structure of our stellar universe; but he considers that we are as yet
comparatively ignorant of the internal structure of either the stellar
or the nebular zones. The structure of the stellar universe, according
to this view, is shown in Fig. 460.

[Illustration: Fig. 460.]




                                 INDEX


 A.

 Aberration of light, 38.

 Aerolites, 304.

 Aldebaran, star in Taurus, 340, 342.

 Algol, a variable star, 343, 358.

 Almanac, perpetual, 82.

 Alps, lunar mountains, 126.

 Altair, star in Aquila, 336.

 Alt-azimuth instrument, 13.

 Altitude, 12.

 Andromeda (constellation), 343, 346.
   nebula in, 376.

 Angström's map of spectrum, 164.

 Antares, star in Scorpio, 347.

 Apennines, lunar mountains, 122, 124.

 Aphelion, 47.

 Apogee, 44.

 Aquarius, or the Water-Bearer, 350.
   cluster in, 354.

 Aquila, or the Eagle, 336.

 Arcturus, star in Boötes, 335, 365, 370.

 Argo, or the Ship, 360.
   nebula in, 383.
   variable star in, 360.

 Aries, or the Ram, 350.

 Asteroids, 223, 241.

 Astræa, an asteroid, 241.

 Auriga, or the Wagoner, 342.

 Azimuth, 13.


 B.

 Betelgeuse, star in Orion, 340, 370.

 Berenice's Hair (constellation), 334.

 Bode's law, 241.
   disproved, 273.

 Boötes (constellation), 334, 335.


 C.

 Calendar, the, 80.

 Callisto, moon of Jupiter, 250.

 Cancer, or the Crab, 350.
   tropic of, 61.

 Canes Venatici, or the Hunting-Dogs, 334.

 Canes Venatici, nebula in, 384.

 Canis Major, or the Great Dog, 342.

 Canis Minor, or the Little Dog, 340.

 Capella, star in Auriga, 340, 343.

 Capricorn, tropic of, 61.

 Capricornus, or the Goat, 350.

 Cassiopeia (constellation), 332.
   new star in, 362.

 Castor, star in Gemini, 340, 370.

 Caucasus, a lunar range, 124.

 Centaurus, star-cluster in, 355.

 Cepheus (constellation), 334.
   nebula in, 387.

 Ceres, the planet, 241.

 Cetus, or the Whale, 346.
   variable star in, 359.

 Charles's Wain, 330.

 Circles, great, 4.
   diurnal, 8.
   hour, 16.
   small, 4.
   vertical, 12.

 Clock, astronomical, 18.
   time, 78.

 Coma Berenices, or Berenice's Hair, 334.

 Comet, Biela's, 293.
   and earth, collision of, 316.
   Coggia's, 297.
   Donati's, 296.
   Encke's, 293.
   Halley's, 291.
   of 1680, 290.
   of 1811, 290.
   of 1843, 295.
   of 1861, 297.
   of June, 1881, 300.

 Comets, appearance of, 274.
   and meteors, 313.
   bright, 274.
   chemical constitution of, 318.
   development of, 277.
   number of, 288.
   orbits of, 282.
   origin of, 287.
   periodic, 286.
   physical constitution of, 314.
   tails of, 279.
   telescopic, 275, 281.
   visibility of, 281.

 Conic sections, 48.

 Conjunction, 91.
   inferior, 130.
   superior, 130, 136.

 Constellations, 325.
   zodiacal, 32.

 Copernican system, the, 44, 53.

 Copernicus, a lunar crater, 120, 129.

 Corona Borealis, or the Northern Crown, 336.

 Corona Borealis, new star in, 363.

 Corvus, or the Crow, 339.

 Crystalline spheres, 41.

 Cycles and epicycles, 42.

 Cygnus, or the Swan, 338.


 D.

 Day and night, 57.
   civil, 77.
   lunar, 108.
   sidereal, 74.
   solar, 74.

 Declination, 16.

 Deimos, satellite of Mars, 239.

 Delphinus, or the Dolphin, 338.

 Deneb, star in Cygnus, 338, 370.

 Dione, satellite of Saturn, 259.

 Dipper, the Great, 330, 366, 369, 370.
   the Little, 331.
   the Milk, 347.

 Dissociation, 163.

 Dominical Letter, the, 81.

 Draco, or the Dragon, 331.


 E.

 Earth, density of, 85.
   flattened at poles, 55.
   form of, 53.
   in space, 56.
   seen from moon, 109.
   size of, 55.
   weight of, 83.

 Eccentric, the 43.

 Eccentricity, 46.

 Eclipses, 210.
   annular, 219.
   lunar, 210, 214.
   solar, 216.

 Ecliptic, the, 27.
   obliquity of, 28.

 Ellipse, the, 45, 49.

 Elongation, of planet, 130.

 Enceladus, moon of Saturn, 259.

 Epicycles, 42.

 Epicycloid, 107.

 Epsilon Lyræ, a double star, 356.

 Equator, the celestial, 7.

 Equinoctial, the, 7.
   colure, 16.
   elevation of, 9.

 Equinox, autumnal, 29.
   vernal, 16, 29.

 Equinoxes, precession of, 31, 85.

 Eta Argus, a variable star, 360, 383.

 Europa, moon of Jupiter, 250.

 F.

 Faculæ, solar, 177.

 Fomalhaut, star in Southern Fish, 350.

 Fraunhofer's lines, 164, 371.


 G.

 Galaxy, the, 326.

 Ganymede, moon of Jupiter, 250.

 Gemini, or the Twins, 340.

 Georgium Sidus, 271.


 H.

 Hercules (constellation), 336.
   cluster in, 353.
   orbit of double star in, 357.
   solar system moving towards, 367.

 Herschel, the planet (see Uranus).

 Herschel's hypothesis, 392, 396.

 Horizon, the, 5.

 Hyades, the, 342, 350.

 Hydra, or the Water-Snake, 340.

 Hyperbola, the, 49.

 Hyperion, moon of Saturn, 259.


 I.

 Io, moon of Jupiter, 250.

 Irradiation, 90, 113.


 J.

 Japetus, moon of Saturn, 259.

 Job's Coffin (asterism), 338.

 Juno, the planet, 241.

 Jupiter, apparent size of, 245.
   distance of, 245.
   great red spot of, 249.
   orbit of, 244.
   periods of, 246.
   physical constitution of, 246.
   rotation of, 248.
   satellites of, 250.
     eclipses of, 252.
     transits of, 254.
   volume of, 245.
   without satellites, 255.


 K.

 Kant's hypothesis, 391.

 Kepler, a lunar crater, 129.

 Kepler's system, 44.
   laws, 46.
   star, 362.

 Kirchhoff's map of spectrum, 164.

 L.

 Laplace's hypothesis, 392.

 Latitude, celestial, 30.

 Leap year, 81.

 Leo, or the Lion, 334.

 Leonids (meteors), 312.

 Libra, or the Balances, 347.

 Libration, 102.

 Longitude, celestial, 30.

 Lyra, or the Lyre, 338.
   double star in, 356.


 M.

 Magellanic clouds, the, 389.

 Magnetic storms, 190.

 Magnetism and sun-spots, 190.

 Mars, apparent size of, 236.
   brilliancy of, 237.
   distance of, 235.
   orbit of, 235.
   periods of, 237.
   rotation of, 239.
   satellites of, 239.
   volume of, 236.

 Mercury, apparent size of, 226.
   atmosphere of, 228.
   distance of, 225.
   elongation of, 227.
   orbit of, 225.
   periods of, 227.
   volume of, 226.

 Meridian, the, 12.

 Meridian circle, 17.

 Meridians, celestial, 31.

 Meteoric iron, 305, 307.
   showers, 310.
   stones, 305.

 Meteors, 300.
   August, 311.
   light of, 309.
   November, 312.
   sporadic, 310.

 Meteoroids, 308.

 Micrometers, 20, 153.

 Milky-Way, the, 326.

 Mimas, moon of Saturn, 259.

 Mira, a variable star, 359.

 Moon, apparent size of, 87, 89.
   aspects of, 91.
   atmosphere of, 109.
   chasms in, 123.
   craters in, 119.
   day of, 108.
   distance of, 86.
   eclipses of, 210.
   form of orbit, 97.
   harvest, 101.
   hunter's, 102.
   inclination of orbit, 97.
   kept in her path by gravity, 51.
   librations of, 102.
   mass of, 90.
   meridian altitude of, 98.
   mountains of, 116.
   orbital motion of, 91.
   phases of, 93.
   real size of, 88.
   rising of, 99.
   rotation of, 102.
   sidereal period of, 92.
   surface of, 115.
   synodical period of, 92.
   terminator of, 115.
   wet and dry, 98.


 N.

 Nadir, the, 6.

 Neap-tides, 72.

 Nebula, in Andromeda, 376.
   crab, 376.
   dumb-bell, 383.
   in Argus, 383.
   in Canes Venatici, 384.
   in Cepheus, 387.
   in Orion, 378.
   in the Triangle, 387.
   in Ursa Major, 386.

 Nebulæ, 281, 330, 373.
   annular, 373.
   circular, 373.
   condensation of, 385.
   double, 375.
   elliptical, 373.
   irregular, 376.
   multiple, 375.
   spiral, 373, 384.

 Nebular hypothesis, the, 391.

 Neptune, discovery of, 271.
   orbit of, 271.
   satellite of, 274.

 New style, 80.

 Newcomb's theory of the stellar universe, 398.

 Newton's system, 48.

 Nodes, 97.

 Nubecula, Major, 389.
   Minor, 389.

 Nutation, 34.


 O.

 Olbers's hypothesis, 241.

 Old style, 80.

 Ophiuchus (constellation), 347.
   new star in, 362.

 Opposition, 91, 136.

 Orion, 341.
   nebula in, 378.
   the trapezium of, 356.


 P.

 Pallas, the planet, 241.

 Parabola, the, 49.

 Parallax, 37.

 Pegasus (constellation), 343, 346.
   triple star in, 356.

 Perigee, 44.

 Perihelion, 47.

 Perseids (meteors), 311.

 Perseus (constellation), 346.
   cluster in, 353.

 Phobos, satellite of Mars, 239.

 Pico, a lunar mountain, 127.

 Pisces, or the Fishes, 350.

 Piscis Australis, or the Southern Fish, 350.

 Planets, 39.
   inferior, 130.
     periods of, 132.
     phases of, 132.
   inner group of, 221.
   intra-Mercurial, 230.
   minor, 223.
   outer group of, 222, 244.
   superior, 134.
     motion of, 134.
     periods of, 137.
     phases of, 137.
   three groups of, 221.

 Pleiades, the, 328, 342, 351.

 Pointers, the, 330.

 Polar distance, 16.

 Pole Star, the, 7, 330, 365.

 Poles, celestial, 7, 9.

 Pollux, star in Gemini, 340, 370.

 Præsepe, or the Beehive, 350.

 Precession of equinoxes, 31, 85.

 Prime vertical, the, 12.

 Proctor's theory of the stellar universe, 398.

 Procyon, star in Canis Minor, 340.

 Ptolemaic system, the, 41.


 Q.

 Quadrature, 91, 137.


 R.

 Radiant point (meteors), 310.

 Radius vector, 47.

 Refraction, 35.

 Regulus, star in Leo, 334, 370.

 Rhea, moon of Saturn, 259.

 Rigel, star in Orion, 340, 370.

 Right ascension, 16.


 S.

 Sagittarius, or the Archer, 347.

 Saturn, apparent size of, 256.
   distance of, 256.
   orbit of, 255.
   periods of, 256.
   physical constitution of, 257.
   ring of, 261.
     changes in, 268.
     constitution of, 269.
     phases of, 263.
   rotation of, 258.
   satellites of, 259.
   volume of, 256.

 Scorpio, or the Scorpion, 347.
   cluster in, 355.

 Seasons, the, 64.

 Sirius, the Dog-Star, 340, 342, 365, 370, 371.

 Solar system, the, 41.

 Solstices, 29, 59, 60.

 Sound, effect of motion on, 168.

 Spectra, bright-lined, 158.
   comparison of, 154.
   continuous, 158.
   displacement of lines in, 171.
   of comets, 318.
   reversed, 161.
   sun-spot, 193.
   types of stellar, 371.

 Spectroscope, the, 152.
   diffraction, 157.
   direct-vision, 155.
   dispersion, 152.

 Spectrum analysis, 159.
   solar, 164.

 Sphere, defined, 3.
   the celestial, 5.
     rotation of, 7.

 Spring-tides, 72.

 Stars, circumpolar, 7.
   clusters of, 328, 350.
   color of, 357.
   constellations of, 325.
   constitution of, 371.
   distance of, 364.
   double, 355.
   drift of, 368.
   four sets of, 10.
   magnitude of, 322.
   motion of, in line of sight, 369.
   multiple, 356.
   names of, 325.
   nebulous, 373.
   new, 361.
   number of, 323.
   parallax of, 364.
   proper motion of, 365.
   secular displacement of, 366.
   temporary, 361.
   variable, 358.

 Sun, atmosphere of, 149.
   brightness of, 151.
   chemical constitution of, 164.
   chromosphere of, 149, 196.
   corona of, 149, 196, 204.
   distance of, 142.
   faculæ of, 177.
   heat radiated by, 150.
   inclination of axis of, 187.
   mass of, 140.
   motion of, among the stars, 26.
     at surface of, 168.
     in atmosphere of, 172.
     secular, 366.
   photosphere of, 149, 175.
   prominences of, 149, 197.
   rotation of, 186.
   spectrum of, 164, 171.
   temperature of, 149.
   volume of, 140.
   winds on, 174.

 Sun-spots, 179.
   and magnetism, 190.
   birth and decay of, 185.
   cause of, 194.
   cyclonic motion in, 182.
   distribution of, 188.
   duration of, 181.
   groups of, 181.
   periodicity of, 189.
   proper motion of, 187.
   size of, 181.
   spectrum of, 193.


 T.

 Taurus, or the Bull, 342.
   quadruple star in, 356.

 Telescope, Cassegrainian, 23.
   equatorial, 19.
   front-view, 22.
   Gregorian, 23.
   Herschelian, 22.
   Lord Rosse's, 25.
   Melbourne, 25.
   Newall, 20.
   Newtonian, 22.
   Paris, 26.
   reflecting, 21.
   Washington, 20.
   Vienna, 20.

 Telespectroscope, the, 155.

 Telluric lines of spectrum, 165.

 Tethys, moon of Saturn, 259.

 Tides, 67.

 Time, clock, 78.
   sun, 78.

 Titan, moon of Saturn, 259, 261.

 Toucan, star cluster in, 354, 389.

 Transit instrument, 17.

 Transits of Venus, 145.

 Triesneker, lunar formation, 123.

 Tropics, 61.

 Twilight, 62.

 Tycho Brahe's star, 361.
   system, 44.

 Tycho, a lunar crater, 129.


 U.

 Universe, structure of the stellar, 396.


 Uranus, discovery of, 271.
   name of, 270.
   orbit of, 269.
   satellites of, 271.

 Ursa Major, or the Great Bear, 330.
   nebula in, 386.

 Ursa Minor, or the Little Bear, 330.


 V.

 Vega, star in Lyra, 336, 365, 370.

 Venus, apparent size of, 231.
   atmosphere of, 234.
   brilliancy of, 232.
   distance of, 231.
   elongation of, 231.
   orbit of, 230.
   periods of, 232.
   volume of, 231.
   transits of, 145, 234.

 Vernier, the, 15.

 Virgo, or the Virgin, 338.

 Vesta, the planet, 241.

 Vulcan, the planet, 230.


 Y.

 Year, the, 78.
   anomalistic, 79.
   Julian, 80.
   sidereal, 79.
   tropical, 79.


 Z.

 Zenith, the, 6.
   distance, 12.

 Zodiac, the, 32.

 Zodiacal constellations, 32.
   light, 318.

 Zones, 61.




      *      *      *      *      *      *




Transcriber's note:

Missing or obscured punctuation was corrected.

Typographical errors were silently corrected.





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