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diff --git a/old/48218-h/48218-h.htm b/old/48218-h/48218-h.htm new file mode 100644 index 0000000..b70e38e --- /dev/null +++ b/old/48218-h/48218-h.htm @@ -0,0 +1,4485 @@ +<!DOCTYPE html PUBLIC "-//W3C//DTD XHTML 1.1//EN" + "http://www.w3.org/TR/xhtml11/DTD/xhtml11.dtd"> + +<html xmlns="http://www.w3.org/1999/xhtml" xml:lang="en"> + +<head> + +<link rel="coverpage" href="images/img-cover.jpg" /> + +<meta http-equiv="Content-Type" content="text/html; charset=ISO-8859-1" /> + +<title> +The Project Gutenberg E-text of The Science of the Stars, +by E. Walter Maunder +</title> + +<style type="text/css"> +body { color: black; + background: white; + margin-right: 10%; + margin-left: 10%; + font-family: "Times New Roman", serif; + text-align: justify } + +p {text-indent: 4% } + +p.noindent {text-indent: 0% } + +p.t1 {text-indent: 0% ; + font-size: 200%; + text-align: center } + +p.t2 {text-indent: 0% ; + font-size: 150%; + text-align: center } + +p.t2b {text-indent: 0% ; + font-size: 150%; + font-weight: bold; + text-align: center } + +p.t3 {text-indent: 0% ; + font-size: 100%; + text-align: center } + +p.t3b {text-indent: 0% ; + font-size: 100%; + font-weight: bold; + text-align: center } + +p.t4 {text-indent: 0% ; + font-size: 80%; + text-align: center } + +p.t4b {text-indent: 0% ; + font-size: 80%; + font-weight: bold; + text-align: center } + +p.t5 {text-indent: 0% ; + font-size: 60%; + text-align: center } + +h1 { text-align: center } +h2 { text-align: center } +h3 { text-align: center } +h4 { text-align: center } +h5 { text-align: center } + +p.poem {text-indent: 0%; + margin-left: 10%; } + +p.contents {text-indent: -3%; + margin-left: 5% } + +p.thought {text-indent: 0% ; + letter-spacing: 4em ; + text-align: center } + +p.letter {text-indent: 0%; + margin-left: 10% ; + margin-right: 10% } + +p.footnote {text-indent: 0% ; + font-size: 80%; + margin-left: 10% ; + margin-right: 10% } + +pre.index { font-family: "Times New Roman", serif; + font-size: 100% } + +p.finis { font-size: larger ; + text-align: center ; + text-indent: 0% ; + margin-left: 0% ; + margin-right: 0% } + +.pagenum { position: absolute; + left: 1%; + font-size: 95%; + text-align: left; + text-indent: 0; + font-style: normal; + font-weight: normal; + font-variant: normal; } + +</style> + +</head> + +<body> + + +<pre> + +The Project Gutenberg EBook of The Science of the Stars, by E. Walter Maunder + +This eBook is for the use of anyone anywhere in the United States and most +other parts of the world at no cost and with almost no restrictions +whatsoever. You may copy it, give it away or re-use it under the terms of +the Project Gutenberg License included with this eBook or online at +www.gutenberg.org. If you are not located in the United States, you'll have +to check the laws of the country where you are located before using this ebook. + +Title: The Science of the Stars + +Author: E. Walter Maunder + +Release Date: February 9, 2015 [EBook #48218] + +Language: English + +Character set encoding: ISO-8859-1 + +*** START OF THIS PROJECT GUTENBERG EBOOK THE SCIENCE OF THE STARS *** + + + + +Produced by Al Haines + + + + + +</pre> + + +<h1> +<br /><br /><br /> +THE SCIENCE OF +THE STARS +</h1> + +<p><br /></p> + +<p class="t2"> +BY E. WALTER MAUNDER, F.R.A.S. +</p> + +<p class="t4"> +OF THE ROYAL OBSERVATORY, GREENWICH +</p> + +<p class="t4"> +AUTHOR OF "ASTRONOMY WITHOUT A TELESCOPE"<br /> +"THE ASTRONOMY OF THE BIBLE," ETC. +</p> + +<p><br /><br /></p> + +<p class="t3"> +LONDON: T. C. & E. C. JACK<br /> +67 LONG ACRE, W.C., AND EDINBURGH<br /> +NEW YORK: DODGE PUBLISHING CO.<br /> +</p> + +<p><br /><br /><br /></p> + +<p> +<span class="pagenum">{<a id="Pvii"></a>vii}</span> +</p> + +<p class="t3b"> +CONTENTS +</p> + +<p class="noindent"> +CHAP. +</p> + +<p class="noindent"> +I. <a href="#chap01">ASTRONOMY BEFORE HISTORY</a><br /> +II. <a href="#chap02">ASTRONOMY BEFORE THE TELESCOPE</a><br /> +III. <a href="#chap03">THE LAW OF GRAVITATION</a><br /> +IV. <a href="#chap04">ASTRONOMICAL MEASUREMENTS</a><br /> +V. <a href="#chap05">THE MEMBERS OF THE SOLAR SYSTEM</a><br /> +VI. <a href="#chap06">THE SYSTEM OF THE STARS</a><br /> +<a href="#chap08">INDEX</a> +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap01"></a></p> + +<p><span class="pagenum">{<a id="P9"></a>9}</span></p> + +<p class="t2b"> +THE SCIENCE OF THE STARS +</p> + +<p><br /><br /></p> + +<h3> +CHAPTER I +</h3> + +<h3> +ASTRONOMY BEFORE HISTORY +</h3> + +<p> +The plan of the present series requires each volume +to be complete in about eighty small pages. But no +adequate account of the achievements of astronomy +can possibly be given within limits so narrow, for so +small a space would not suffice for a mere catalogue of +the results which have been obtained; and in most +cases the result alone would be almost meaningless +unless some explanation were offered of the way in +which it had been reached. All, therefore, that can be +done in a work of the present size is to take the student +to the starting-point of astronomy, show him the various +roads of research which have opened out from it, and +give a brief indication of the character and general +direction of each. +</p> + +<p> +That which distinguishes astronomy from all the +other sciences is this: it deals with objects that we +cannot touch. The heavenly bodies are beyond our +reach; we cannot tamper with them, or subject them +to any form of experiment; we cannot bring them into +our laboratories to analyse or dissect them. We can +only watch them and wait for such indications as their +<span class="pagenum">{<a id="P10"></a>10}</span> +own movements may supply. But we are confined to +this earth of ours, and they are so remote; we are so +short-lived, and they are so long-enduring; that the +difficulty of finding out much about them might well +seem insuperable. +</p> + +<p> +Yet these difficulties have been so far overcome that +astronomy is the most advanced of all the sciences, the +one in which our knowledge is the most definite and +certain. All science rests on sight and thought, on +ordered observation and reasoned deduction; but both +sight and thought were earlier trained to the service of +astronomy than of the other physical sciences. +</p> + +<p> +It is here that the highest value of astronomy lies; +in the discipline that it has afforded to man's powers +of observation and reflection; and the real triumphs +which it has achieved are not the bringing to light of +the beauties or the sensational dimensions and distances +of the heavenly bodies, but the vanquishing of +difficulties which might well have seemed superhuman. +The true spirit of the science can be far better +exemplified by the presentation of some of these difficulties, +and of the methods by which they have been overcome, +than by many volumes of picturesque description +or of eloquent rhapsody. +</p> + +<p> +There was a time when men knew nothing of +astronomy; like every other science it began from zero. +But it is not possible to suppose that such a state of +things lasted long, we know that there was a time +when men had noticed that there were two great lights +in the sky—a greater light that shone by day, a lesser +light that shone by night—and there were the stars +also. And this, the earliest observation of primitive +astronomy, is preserved for us, expressed in the simplest +possible language, in the first chapter of the first book +<span class="pagenum">{<a id="P11"></a>11}</span> +of the sacred writings handed down to us by the +Hebrews. +</p> + +<p> +This observation, that there are bodies above us +giving light, and that they are not all equally bright, +is so simple, so inevitable, that men must have made +it as soon as they possessed any mental power at all. +But, once made, a number of questions must have +intruded themselves: "What are these lights? Where +are they? How far are they off?" +</p> + +<p> +Many different answers were early given to these +questions. Some were foolish; some, though +intelligent, were mistaken; some, though wrong, led +eventually to the discovery of the truth. Many myths, many +legends, some full of beauty and interest, were invented. +But in so small a book as this it is only possible to +glance at those lines of thought which eventually led +to the true solution. +</p> + +<p> +As the greater light, the lesser light, and the stars +were carefully watched, it was seen not only that they +shone, but that they appeared to move; slowly, steadily, +and without ceasing. The stars all moved together like +a column of soldiers on the march, not altering their +positions relative to each other. The lesser light, the +Moon, moved with the stars, and yet at the same time +among them. The greater light, the Sun, was not seen +with the stars; the brightness of his presence made +the day, his absence brought the night, and it was +only during his absence that the stars were seen; they +faded out of the sky before he came up in the morning, +and did not reappear again until after he passed out +of sight in the evening. But there came a time when +it was realised that there were stars shining in the sky +all day long as well as at night, and this discovery was +one of the greatest and most important ever made, +<span class="pagenum">{<a id="P12"></a>12}</span> +because it was the earliest discovery of something quite +unseen. Men laid hold of this fact, not from the direct +and immediate evidence of their senses, but from +reflection and reasoning. We do not know who made +this discovery, nor how long ago it was made, but from +that time onward the eyes with which men looked +upon nature were not only the eyes of the body, but +also the eyes of the mind. +</p> + +<p> +It followed from this that the Sun, like the Moon, +not only moved with the general host of the stars, +but also among them. If an observer looks out from +any fixed station and watches the rising of some bright +star, night after night, he will notice that it always +appears to rise in the same place; so too with its +setting. From any given observing station the direction +in which any particular star is observed to rise or +set is invariable. +</p> + +<p> +Not so with the Sun. We are accustomed to say +that the Sun rises in the east and sets in the west. But +the direction in which the Sun rises in midwinter lies +far to the south of the east point; the direction in which +he rises in midsummer lies as far to the north. The +Sun is therefore not only moving with the stars, but +among them. This gradual change in the position of +the Sun in the sky was noticed in many ancient nations +at an early time. It is referred to in Job xxxviii. 12: +"Hast thou commanded the morning since thy days; +and caused the dayspring to know his place?" +</p> + +<p> +And the apparent path of the Sun on one day is +always parallel to its path on the days preceding and +following. When, therefore, the Sun rises far to the +south of east, he sets correspondingly far to the south +of west, and at noon he is low down in the south. His +course during the day is a short one, and the daylight +<span class="pagenum">{<a id="P13"></a>13}</span> +is much shorter than the night, and the Sun at noon, +being low down in the sky, has not his full power. The +cold and darkness of winter, therefore, follows directly +upon this position of the Sun. These conditions are +reversed when the Sun rises in the north-east. The +night is short, the daylight prolonged, and the Sun, +being high in the heavens at noon, his heat is felt to +the full. +</p> + +<p> +Thus the movements of the Sun are directly +connected with the changes of season upon the Earth. +But the stars also are connected with those seasons; +for if we look out immediately after it has become dark +after sunset, we shall notice that the stars seen in the +night of winter are only in part those seen in the nights +of summer. +</p> + +<p> +In the northern part of the sky there are a number +of stars which are always visible whenever we look out, +no matter at what time of the night nor what part of the +year. If we watch throughout the whole night, we see +that the whole heavens appear to be slowly turning—turning, +as if all were in a single piece—and the pivot +about which it is turning is high up in the northern +sky. The stars, therefore, are divided into two classes. +Those near this invisible pivot—the "Pole" of the +Heavens, as we term it—move round it in complete +circles; they never pass out of sight, but even when +lowest they clear the horizon. The other stars move +round the same pivot in curved paths, which are +evidently parts of circles, but circles of which we do not +see the whole. These stars rise on the eastern side of +the heavens and set on the western, and for a greater +or less space of time are lost to sight below the horizon. +And some of these stars are visible at one time of the +year, others at another; some being seen during the +<span class="pagenum">{<a id="P14"></a>14}</span> +whole of the long nights of winter, others throughout +the short nights of summer. This distinction again, +and its connection with the change of the seasons on +the earth, was observed many ages ago. It is alluded +to in Job xxxviii. 32: "Canst thou lead forth the +Signs of the Zodiac in their season, or canst thou guide +the Bear with her train?" (R.V., Margin). The Signs +of the Zodiac are taken as representing the stars which +rise and set, and therefore have each their season for +being "led forth," while the northern stars, which are +always visible, appearing to be "guided" in their +continual movement round the Pole of the sky in perfect +circles, are represented by "the Bear with her train." +</p> + +<p> +The changes in position of the Sun, the greater light, +must have attracted attention in the very earliest ages, +because these changes are so closely connected with +the changes of the seasons upon the Earth, which affect +men directly. The Moon, the lesser light, goes through +changes of position like the Sun, but these are not of +the same direct consequence to men, and probably +much less notice was taken of them. But there were +changes of the Moon which men could not help noticing—her +changes of shape and brightness. One evening she +may be seen soon after the Sun has set, as a thin arch +of light, low down in the sunset sky. On the following +evenings she is seen higher and higher in the sky, +and the bow of light increases, until by the fourteenth +day it is a perfect round. Then the Moon begins to +diminish and to disappear, until, on the twenty-ninth +or thirtieth day after the first observation, she is again +seen in the west after sunset as a narrow crescent. This +succession of changes gave men an important measure +of time, and, in an age when artificial means of light +were difficult to procure, moonlight was of the greatest +<span class="pagenum">{<a id="P15"></a>15}</span> +value, and the return of the moonlit portion of the +month was eagerly looked for. +</p> + +<p> +These early astronomical observations were simple +and obvious, and of great practical value. The day, +month, and year were convenient measures of time, and +the power of determining, from the observation of the +Sun and of the stars, how far the year had progressed +was most important to farmers, as an indication when +they should plough and sow their land. Such +observations had probably been made independently by +many men and in many nations, but in one place a +greater advance had been made. The Sun and Moon +are both unmistakable, but one star is very like +another, and, for the most part, individual stars can +only be recognised by their positions relative to others. +The stars were therefore grouped together into +<b>Constellations</b> and associated with certain fancied designs, +and twelve of these designs were arranged in a belt +round the sky to mark the apparent path of the Sun +in the course of the year, these twelve being known as +the "<b>Signs of the Zodiac</b>"—the Ram, Bull, Twins, Crab, +Lion, Virgin, Balance, Scorpion, Archer, Goat, Water-pourer, +and Fishes. In the rest of the sky some thirty +to thirty-six other groups, or constellations, were formed, +the Bear being the largest and brightest of the +constellations of the northern heavens. +</p> + +<p> +But these ancient constellations do not cover the +entire heavens; a large area in the south is untouched +by them. And this fact affords an indication both of +the time when and the place where the old stellar groups +were designed, for the region left untouched was the +region below the horizon of 40° North latitude, about +4600 years ago. It is probable, therefore, that the +ancient astronomers who carried out this great work +<span class="pagenum">{<a id="P16"></a>16}</span> +lived about 2700 B.C., and in North latitude 37° or 38°. +The indication is only rough, but the amount of +uncertainty is not very large; the constellations must be at +least 4000 years old, they cannot be more than 5000. +</p> + +<p> +All this was done by prehistoric astronomers; though +no record of the actual carrying out of the work and +no names of the men who did it have come down to +us. But it is clear from the fact that the Signs of the +Zodiac are arranged so as to mark out the annual path +of the Sun, and that they are twelve in number—there +being twelve months in the year—that those who +designed the constellations already knew that there are +stars shining near the Sun in full daylight, and that +they had worked out some means for determining what +stars the Sun is near at any given time. +</p> + +<p> +Another great discovery of which the date and the +maker are equally unknown is referred to in only one +of the ancient records available to us. It was seen that +all along the eastern horizon, from north to south, stars +rise, and all along the western horizon, from north to +south, stars set. That is what was seen; it was the +fact observed. There is no hindrance anywhere to the +movement of the stars—they have a free passage under +the Earth; the Earth is unsupported in space. That +is what was <i>thought</i>; it was the inference drawn. Or, +as it is written in Job xxvi. 7, "He (God) stretcheth +out the north over empty space, and hangeth the earth +upon nothing." +</p> + +<p> +The Earth therefore floats unsupported in the centre +of an immense star-spangled sphere. And what is the +shape of the Earth? The natural and correct inference +is that it is spherical, and we find in some of the early +Greek writers the arguments which establish this +inference as clearly set forth as they would be to-day. +<span class="pagenum">{<a id="P17"></a>17}</span> +The same inference followed, moreover, from the +observation of a simple fact, namely, that the stars as +observed from any particular place all make the same +angle with the horizon as they rise in the east, and all +set at the same angle with it in the west; but if we go +northward, we find that angle steadily decreasing; if +we go southward, we find it increasing. But if the Earth +is round like a globe, then it must have a definite size, +and that size can be measured. The discoveries noted +above were made by men whose names have been lost, +but the name of the first person whom we know to have +measured the size of the Earth was ERATOSTHENES. +He found that the Sun was directly overhead at noon at +midsummer at Syene (the modern Assouan), in Egypt, +but was 7° south of the "zenith"—the point +overhead—at Alexandria, and from this he computed the +Earth to be 250,000 stadia (a stadium = 606 feet) in +circumference. +</p> + +<p> +Another consequence of the careful watch upon the +stars was the discovery that five of them were planets; +"wandering" stars; they did not move all in one +piece with the rest of the celestial host. In this they +resemble the Sun and Moon, and they further resemble +the Moon in that, though too small for any change of +shape to be detected, they change in brightness from +time to time. But their movements are more +complicated than those of the other heavenly bodies. The +Sun moves a little slower than the stars, and so seems +to travel amongst them from west to east; the Moon +moves much slower than the stars, so her motion from +west to east is more pronounced than that of the Sun. +But the five planets sometimes move slower than the +stars, sometimes quicker, and sometimes at the same +rate. Two of the five, which we now know as Mercury +<span class="pagenum">{<a id="P18"></a>18}</span> +and Venus, never move far from the Sun, sometimes +being seen in the east before he rises in the morning, +and sometimes in the west after he has set in the +evening. Mercury is the closer to the Sun, and moves +more quickly; Venus goes through much the greater +changes of brightness. Jupiter and Saturn move +nearly at the same average rate as the stars, Saturn +taking about thirteen days more than a year to come +again to the point of the sky opposite to the Sun, and +Jupiter about thirty-four days. Mars, the fifth planet, +takes two years and fifty days to accomplish the same +journey. +</p> + +<p> +These planetary movements were not, like those of +the Sun and Moon and stars, of great and obvious +consequence to men. It was important to men to know +when they would have moonlight nights, to know +when the successive seasons of the year would return. +But it was no help to men to know when Venus was +at her brightest more than when she was invisible. +She gave them no useful light, and she and her +companion planets returned at no definite seasons. +Nevertheless, men began to make ordered observations of the +planets—observations that required much more patience +and perseverance than those of the other celestial +lights. And they set themselves with the greatest +ingenuity to unravel the secret of their complicated and +seemingly capricious movements. +</p> + +<p> +This was a yet higher development than anything +that had gone before, for men were devoting time, +trouble, and patient thought, for long series of years, +to an inquiry which did not promise to bring them any +profit or advantage. Yet the profit which it actually +did bring was of the highest order. It developed +men's mental powers; it led to the devising of +<span class="pagenum">{<a id="P19"></a>19}</span> +instruments of precision for the observations; it led +to the foundation of mathematics, and thus lay at the +root of all our modern mechanical progress. It brought +out, in a higher degree, ordered observation and ordered +thought. +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap02"></a></p> + +<p><span class="pagenum">{<a id="P20"></a>20}</span></p> + +<h3> +CHAPTER II +</h3> + +<h3> +ASTRONOMY BEFORE THE TELESCOPE +</h3> + +<p> +There was thus a real science of astronomy before we +have any history of it. Some important discoveries +had been made, and the first step had been taken +towards cataloguing the fixed stars. It was certainly +known to some of the students of the heavens, though +perhaps only to a few, that the Earth was a sphere, +freely suspended in space, and surrounded on all sides +by the starry heavens, amongst which moved the Sun, +Moon, and the five planets. The general character of +the Sun's movement was also known; namely, that he +not only moved day by day from east to west, as the +stars do, but also had a second motion inclined at an +angle to the first, and in the opposite direction, which +he accomplished in the course of a year. +</p> + +<p> +To this sum of knowledge, no doubt, several nations +had contributed. We do not know to what race we +owe the constellations, but there are evidences of an +elementary acquaintance with astronomy on the part +of the Chinese, the Babylonians, the Egyptians, and +the Jews. But in the second stage of the development +of the science the entire credit for the progress made +belongs to the Greeks. +</p> + +<p> +The Greeks, as a race, appear to have been very +little apt at originating ideas, but they possessed, beyond +all other races, the power of developing and perfecting +crude ideas which they had obtained from other sources, +<span class="pagenum">{<a id="P21"></a>21}</span> +and when once their attention was drawn to the +movements of the heavenly bodies, they devoted +themselves with striking ingenuity and success to devising +theories to account for the appearances presented, to +working out methods of computation, and, last, to +devising instruments for observing the places of the +luminaries in which they were interested. +</p> + +<p> +In the brief space available it is only possible to +refer to two or three of the men whose commanding +intellects did so much to help on the development of +the science. EUDOXUS of Knidus, in Asia Minor +(408-355 B.C.), was, so far as we know, the first to attempt +to represent the movements of the heavenly bodies by +a simple mathematical process. His root idea was +something like this. The Earth was in the centre of the +universe, and it was surrounded, at a great distance from +us, by a number of invisible transparent shells, or +spheres. Each of these spheres rotated with perfect +uniformity, though the speed of rotation differed for +different spheres. One sphere carried the stars, and +rotated from east to west in about 23 h. 56 m. +The Sun was carried by another sphere, which rotated +from west to east in a year, but the pivots, or poles, of +this sphere were carried by a second, rotating exactly +like the sphere of the stars. This explained how it is +that the ecliptic—that is to say, the apparent path of +the Sun amongst the stars—is inclined 23-½° to the +equator of the sky, so that the Sun is 23-½° north of the +equator at midsummer and 23-½° south of the equator +at midwinter, for the poles of the sphere peculiar to +the Sun were supposed to be 23-½° from the poles of the +sphere peculiar to the stars. Then the Moon had three +spheres; that which actually carried the Moon having +its poles 5° from the poles of the sphere peculiar to the +<span class="pagenum">{<a id="P22"></a>22}</span> +Sun. These poles were carried by a sphere placed like +the sphere of the Sun, but rotating in 27 days; and +this, again, had its poles in the sphere of the stars. The +sphere carrying the Moon afforded the explanation of +the wavy motion of the Moon to and fro across the +ecliptic in the course of a month, for at one time in the +month the Moon is 5° north of the ecliptic, at another +time 5° south. The motions of the planets were more +difficult to represent, because they not only have a +general daily motion from east to west, like the stars, +and a general motion from west to east along the +ecliptic, like the Sun and Moon, but from time to time +they turn back on their course in the ecliptic, and +"retrograde." But the introduction of a third and +fourth sphere enabled the motions of most of the planets +to be fairly represented. There were thus twenty-seven +spheres in all—four for each of the five planets, three for +the Moon, three for the Sun (including one not +mentioned in the foregoing summary), and one for the +stars. These spheres were not, however, supposed to +be solid structures really existing; the theory was +simply a means for representing the observed motions +of the heavenly bodies by computations based upon a +series of uniform movements in concentric circles. +</p> + +<p> +But this assumption that each heavenly body moves +in its path at a uniform rate was soon seen to be +contrary to fact. A reference to the almanac will show +at once that the Sun's movement is not uniform. Thus +for the year 1910-11 the solstices and equinoxes fell as +given on the next page: +</p> + +<p> +<span class="pagenum">{<a id="P23"></a>23}</span> +</p> + +<pre> + <i>Epoch Time Interval</i> + + Winter Solstice 1910 Dec. 22 d. 5 h. 12 m. P.M. 89 d. 0 h. 42 m. + Spring Equinox 1911 Mar. 21 " 5 " 54 " P.M. 92 " 19 " 41 " + Summer Solstice 191l June 22 " 1 " 35 " P.M. 93 " 14 " 43 " + Autumn Equinox 1911 Sept. 24 " 4 " 18 " A.M. 89 " 18 " 36 " + Winter Solstice 1911 Dec. 22 " 10 " 54 " P.M. +</pre> + +<p class="noindent"> +so that the winter half of the year is shorter than the +summer half; the Sun moves more quickly over the +half of its orbit which is south of the equator than over +the half which is north of it. +</p> + +<p> +The motion of the Moon is more irregular still, as we +can see by taking out from the almanac the times of +new and full moon: +</p> + +<pre> + <i>New Moon Interval to Full Moon</i> + + Dec. 1910 1 d. 9 h. 10.7 m. P.M. 14 d. 13 h. 54.4 m. + " " 31 " 4 " 21.2 " P.M. 14 " 6 " 4.8 " + Jan. 1911 30 " 9 " 44.7 " A.M. 14 " 0 " 52.8 " + March " 1 " 0 " 31.1 " A.M. 13 " 23 " 27.4 " + " " 30 " 0 " 37.8 " P.M. 14 " 1 " 58.8 " + April " 28 " 10 " 25.0 " P.M. 14 " 7 " 44.7 " + May " 28 " 6 " 24.4 " A.M. 14 " 15 " 26.3 " + June " 26 " 1 " 19.7 " P.M. 14 " 23 " 33.7 " + July " 25 " 8 " 12.0 " P.M. 15 " 6 " 42.7 " + Aug. " 24 " 4 " 14.3 " A.M. 15 " 11 " 42.4 " + Sept. " 22 " 2 " 37.4 " P.M. 15 " 13 " 33.7 " + Oct. " 22 " 4 " 9.3 " A.M. 15 " 11 " 38.8 " + Nov. " 20 " 8 " 49.4 " P.M. 15 " 6 " 2.5 " + Dec. " 20 " 3 " 40.3 " P.M. 14 " 21 " 49.4 " +</pre> + +<p> +<span class="pagenum">{<a id="P24"></a>24}</span> +</p> + +<pre> + <i>Full Moon Interval to New Moon</i> + + Dec. 1910 16 d 11 h. 5.1 m. A.M. 15 d. 5 h. 16.1 m. + Jan. 1911 14 " 10 " 26.0 " P.M. 15 " 11 " 18.7 " + Feb. " 13 " 10 " 37.5 " A.M. 15 " 13 " 53.6 " + March " 14 " 11 " 58.5 " P.M. 15 " 12 " 39.3 " + April " 13 " 2 " 36.6 " P.M. 15 " 7 " 48.4 " + May " 13 " 6 " 9.7 " A.M. 15 " 0 " 14.7 " + June " 11 " 9 " 50.7 " P.M. 14 " 15 " 29.0 " + July " 11 " 0 " 53.4 " P.M. 14 " 7 " 18.6 " + Aug. " 10 " 2 " 54.7 " A.M. 14 " 1 " 19.6 " + Sept. " 8 " 3 " 56.7 " P.M. 13 " 22 " 40.7 " + Oct. " 8 " 4 " 11.1 " A.M. 13 " 23 " 58.2 " + Nov. " 6 " 3 " 48.1 " P.M. 14 " 5 " 1.3 " + Dec. " 6 " 2 " 51.9 " A.M. 14 " 12 " 48.4 " + Jan. 1912 4 " 1 " 99.7 " P.M. 14 " 21 " 40.3 " +</pre> + +<p><br /></p> + +<p> +The astronomer who dealt with this difficulty was +HIPPARCHUS (about 190-120 B.C.), who was born at Nicæa, +in Bithynia, but made most of his astronomical +observations in Rhodes. He attempted to explain these +irregularities in the motions of the Sun and Moon by +supposing that though they really moved uniformly in +their orbits, yet the centre of their orbits was not the +centre of the Earth, but was situated a little distance +from it. This point was called "<b>the excentric</b>," and the +line from the excentric to the Earth was called "<b>the line +of apsides</b>." +</p> + +<p> +But when he tried to deal with the movements of +the planets, he found that there were not enough good +observations available for him to build up any +satisfactory theory. He therefore devoted himself to the +work of making systematic determinations of the places +of the planets that he might put his successors in a +better position to deal with the problem than he was. +His great successor was CLAUDIUS PTOLEMY of +<span class="pagenum">{<a id="P25"></a>25}</span> +Alexandria, who carried the work of astronomical +observation from about A.D. 127 to 150. He was, however, +much greater as a mathematician than as an observer, +and he worked out a very elaborate scheme, by which +he was able to represent the motions of the planets +with considerable accuracy. The system was an +extremely complex one, but its principle may be +represented as follows: If we suppose that a planet is +moving round the Earth in a circle at a uniform rate, +and we tried to compute the place of the planet on this +assumption for regular intervals of time, we should find +that the planet gradually got further and further away +from the predicted place. Then after a certain time +the error would reach a maximum, and begin to +diminish, until the error vanished and the planet was +in the predicted place at the proper time. The error +would then begin to fall in the opposite direction, and +would increase as before to a maximum, subsequently +diminishing again to zero. This state of things might +be met by supposing that the planet was not itself +carried by the circle round the earth, but by an +<b>epicycle</b>—<i>i.e.</i> a circle travelling upon the first circle—and +by judiciously choosing the size of the epicycle and the +time of revolution the bulk of the errors in the planet's +place might be represented. But still there would be +smaller errors going through their own period, and these, +again, would have to be met by imagining that the first +epicycle carried a second, and it might be that the second +carried a third, and so on. +</p> + +<p> +The Ptolemaic system was more complicated than +this brief summary would suggest, but it is not +possible here to do more than indicate the general +principles upon which it was founded, and the numerous +other systems or modifications of them produced in the +<span class="pagenum">{<a id="P26"></a>26}</span> +five centuries from Eudoxus to Ptolemy must be left +unnoticed. The point to be borne in mind is that one +fundamental assumption underlay them all, an assumption +fundamental to all science—the assumption that +like causes must always produce like effects. It was +apparent to the ancient astronomers that the +stars—that is to say, the great majority of the heavenly +bodies—do move round the Earth in circles, and with a +perfect uniformity of motion, and it seemed inevitable +that, if one body moved round another, it should thus +move. For if the revolving body came nearer to the +centre at one time and receded at another, if it moved +faster at one time and slower at another, then, the cause +remaining the same, the effect seemed to be different. +Any complexity introduced by superposing one epicycle +upon another seemed preferable to abandoning this great +fundamental principle of the perfect uniformity of the +actings of Nature. +</p> + +<p> +For more than 1300 years the Ptolemaic system +remained without serious challenge, and the next great +name that it is necessary to notice is that of +COPERNICUS (1473-1543). Copernicus was a canon of +Frauenburg, and led the quiet, retired life of a student. The +great work which made him immortal, <i>De Revolutionibus</i>, +was the result of many years' meditation and work, and +was not printed until he was on his deathbed. In this +work Copernicus showed that he was one of those +great thinkers who are able to look beyond the mere +appearance of things and to grasp the reality of the +unseen. Copernicus realised that the appearance would +be just the same whether the whole starry vault rotated +every twenty-four hours round an immovable Earth +from east to west or the Earth rotated from west to +east in the midst of the starry sphere; and, as the +<span class="pagenum">{<a id="P27"></a>27}</span> +stars are at an immeasurable distance, the latter +conception was much the simpler. Extending the idea of +the Earth's motion further, the supposition that, +instead of the Sun revolving round a fixed Earth in +a year, the Earth revolved round a fixed Sun, made +at once an immense simplification in the planetary +motions. The reason became obvious why Mercury +and Venus were seen first on one side of the Sun and +then on the other, and why neither of them could move +very far from the Sun; their orbits were within the +orbit of the Earth. The stationary points and +retrogressions of the planets were also explained; for, as the +Earth was a planet, and as the planets moved in orbits +of different sizes, the outer planets taking a longer time +to complete a revolution than the inner, it followed, of +necessity, that the Earth in her motion would from +time to time be passed by the two inner planets, and +would overtake the three outer. The chief of the +Ptolemaic epicycles were done away with, and all the +planets moved continuously in the same direction round +the Sun. But no planet's motion could be represented +by uniform motion in a single circle, and Copernicus +had still to make use of systems of epicycles to account +for the deviations from regularity in the planetary +motions round the Sun. The Earth having been +abandoned as the centre of the universe, a further sacrifice +had to be made: the principle of uniform motion in a +circle, which had seemed so necessary and inevitable, +had also to be given up. +</p> + +<p> +For the time came when the instruments for measuring +the positions of the stars and planets had been much +improved, largely due to TYCHO BRAHE (1546-1601), a +Dane of noble birth, who was the keenest and most +careful observer that astronomy had yet produced. +<span class="pagenum">{<a id="P28"></a>28}</span> +His observations enabled his friend and pupil, JOHANN +KEPLER, (1571-1630), to subject the planetary +movements to a far more searching examination than had +yet been attempted, and he discovered that the Sun is +in the plane of the orbit of each of the planets, and +also in its <b>line of apsides</b>—that is to say, the line +joining the two points of the orbit which are respectively +nearest and furthest from the Sun. Copernicus had +not been aware of either of these two relations, but +their discovery greatly strengthened the Copernican +theory. +</p> + +<p> +Then for many years Kepler tried one expedient +after another in order to find a combination of circular +motions which would satisfy the problem before him, +until at length he was led to discard the circle and try +a different curve—the oval or ellipse. Now the +property of a circle is that every point of it is situated at +the same distance from the centre, but in an ellipse +there are two points within it, the "foci," and the sum +of the distances of any point on the circumference from +these two foci is constant. If the two foci are at a +great distance from each other, then the ellipse is very +long and narrow; if the foci are close together, the +ellipse differs very little from a circle; and if we imagine +that the two foci actually coincide, the ellipse becomes +a circle. When Kepler tried motion in an ellipse +instead of motion in a circle, he found that it represented +correctly the motions of all the planets without any +need for epicycles, and that in each case the Sun +occupied one of the foci. And though the planet did not +move at a uniform speed in the ellipse, yet its motion +was governed by a uniform law, for the straight line +joining the planet to the Sun, the "<b>radius vector</b>," passed +over equal areas of space in equal periods of time. +</p> + +<p> +<span class="pagenum">{<a id="P29"></a>29}</span> +</p> + +<p> +These two discoveries are known as Kepler's First +and Second Laws. His Third Law connects all the +planets together. It was known that the outer planets +not only take longer to revolve round the Sun than the +inner, but that their actual motion in space is slower, +and Kepler found that this actual speed of motion is +inversely as the square root of its distance from the +Sun; or, if the square of the speed of a planet be +multiplied by its distance from the Sun, we get the +same result in each case. This is usually expressed by +saying that the cube of the distance is proportional to +the square of the time of revolution. Thus the varying +rate of motion of each planet in its orbit is not only +subject to a single law, but the very different speeds of +the different planets are also all subject to a law that +is the same for all. +</p> + +<p> +Thus the whole of the complicated machinery of +Ptolemy had been reduced to three simple laws, which +at the same time represented the facts of observation +much better than any possible development of the +Ptolemaic mechanism. On his discovery of his third +law Kepler had written: "The book is written to be +read either now or by posterity—I care not which; it +may well wait a century for a reader, as God has waited +6000 years for an observer." Twelve years after his +death, on Christmas Day 1642 (old style), near Grantham, +in Lincolnshire, the predestined "reader" was born. +The inner meaning of Kepler's three laws was brought +to light by ISAAC NEWTON. +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap03"></a></p> + +<p><span class="pagenum">{<a id="P30"></a>30}</span></p> + +<h3> +CHAPTER III +</h3> + +<h3> +THE LAW OF GRAVITATION +</h3> + +<p> +The fundamental thought which, recognised or not, had +lain at the root of the Ptolemaic system, as indeed it +lies at the root of all science, was that "like causes +must always produce like effects." Upon this principle +there seemed to the ancient astronomers no escape +from the inference that each planet must move at a +uniform speed in a circle round its centre of motion. +For, if there be any force tending to alter the distance +of the planet from that centre, it seemed inevitable that +sooner or later it should either reach that centre or be +indefinitely removed from it. If there be no such force, +then the planet's distance from that centre must remain +invariable, and if it move at all, it must move in a +circle; move uniformly, because there is no force either +to hasten or retard it. Uniform motion in a circle +seemed a necessity of nature. +</p> + +<p> +But all this system, logical and inevitable as it had +once seemed, had gone down before the assault of +observed facts. The great example of uniform circular +motion had been the daily revolution of the star +sphere; but this was now seen to be only apparent, +the result of the rotation of the Earth. The planets +revolved round the Sun, but the Sun was not in the +centre of their motion; they moved, not in circles, but +in ellipses; not at a uniform speed, but at a speed +which diminished with the increase of their distance from +<span class="pagenum">{<a id="P31"></a>31}</span> +the Sun. There was need, therefore, for an entire +revision of the principles upon which motion was +supposed to take place. +</p> + +<p> +The mistake of the ancients had been that they +supposed that continued motion demanded fresh applications +of force. They noticed that a ball, set rolling, +sooner or later came to a stop; that a pendulum, set +swinging, might swing for a good time, but eventually +came to rest; and, as the forces that were checking +the motion—that is to say, the friction exercised by the +ground, the atmosphere, and the like—did not obtrude +themselves, they were overlooked. +</p> + +<p> +Newton brought out into clear statement the true +conditions of motion. A body once moving, if acted +upon by no force whatsoever, must continue to move +forward in a straight line at exactly the same speed, +and that for ever. It does not require any maintaining +force to keep it going. If any change in its speed or +in its direction takes place, that change must be due +to the introduction of some further force. +</p> + +<p> +This principle, that, if no force acts on a body in +motion, it will continue to move uniformly in a straight +line, is Newton's First Law of Motion. His Second +lays it down that, if force acts on a body, it produces a +change of motion proportionate to the force applied, +and in the same direction. And the Third Law states +that when one body exerts force upon another, that +second body reacts with equal force upon the first. +The problem of the motions of the planets was, +therefore, not what kept them moving, but what made +them deviate from motion in a straight line, and deviate +by different amounts. +</p> + +<p> +It was quite clear, from the work of Kepler, that the +force deflecting the planets from uniform motion in a +<span class="pagenum">{<a id="P32"></a>32}</span> +straight line lay in the Sun. The facts that the Sun +lay in the plane of the orbits of all the planets, that +the Sun was in one of the foci of each of the planetary +ellipses, that the straight line joining the Sun and +planet moved for each planet over equal areas in equal +periods of time, established this fact clearly. But the +amount of deflection was very different for different +planets. Thus the orbit of Mercury is much smaller +than that of the Earth, and is travelled over in a much +shorter time, so that the distance by which Mercury is +deflected in a course of an hour from movement in a +straight line is much greater than that by which the +Earth is deflected in the same time, Mercury falling +towards the Sun by about 159 miles, whilst the fall of +the Earth is only about 23.9 miles. The force drawing +Mercury towards the Sun is therefore 6.66 times that +drawing the Earth, but 6.66 is the square of 2.58, and +the Earth is 2.58 times as far from the Sun as Mercury. +Similarly, the fall in an hour of Jupiter towards the Sun +is about 0.88 miles, so that the force drawing the Earth +is 27 times that drawing Jupiter towards the Sun. +But 27 is the square of 5.2, and Jupiter is 5.2 times +as far from the Sun as the Earth. Similarly with the +other planets. The force, therefore, which deflects the +planets from motion in a straight line, and compels +them to move round the Sun, is one which varies +inversely as the square of the distance. +</p> + +<p> +But the Sun is not the only attracting body of which +we know. The old Ptolemaic system was correct to a +small extent; the Earth is the centre of motion for the +Moon, which revolves round it at a mean distance of +238,800 miles, and in a period of 27 d. 7 h. 43 m. Hence +the circumference of her orbit is 1,500,450 miles, and +the length of the straight line which she would travel +<span class="pagenum">{<a id="P33"></a>33}</span> +in one second of time, if not deflected by the Earth, is +2828 feet. In this distance the deviation of a circle +from a straight line is one inch divided by 18.66. But +we know from experiment that a stone let fall from a +height of 193 inches above the Earth's surface will +reach the ground in exactly one second of time. The +force drawing the stone to the Earth, therefore, is +193 x 18.66; <i>i.e.</i> 3601 times as great as that drawing +the Moon. But the stone is only 1/330 of a mile from +the Earth's surface, while the Moon is 238,800 miles +away—more than 78 million times as far. The force, +therefore, would seem not to be diminished in the +proportion that the distance is increased—much less +in the proportion of its square. +</p> + +<p> +But Newton proved that a sphere of uniform density, +or made up of any number of concentric shells of uniform +density, attracted a body outside itself, just as if +its entire mass was concentrated at its centre. The +distance of the stone from the Earth must therefore +be measured, not from the Earth's surface, but from +its centre; in other words, we must consider the stone +as being distant from the Earth, not some 16 feet, +but 3963 miles. This is very nearly one-sixtieth of the +Moon's distance, and the square of 60 is 3600. The +Earth's pull upon the Moon, therefore, is almost exactly +in the inverse square of the distance as compared with +its pull on the stone. +</p> + +<p> +Kepler's book had found its "reader." His three +laws were but three particular aspects of Newton's +great discovery that the planets moved under the influence +of a force, lodged in the Sun, which varied inversely +as the square of their distances from it. But Newton's +work went far beyond this, for he showed that the +same law governed the motion of the Moon round the +<span class="pagenum">{<a id="P34"></a>34}</span> +Earth and the motions of the satellites revolving round +the different planets, and also governed the fall of +bodies upon the Earth itself. It was universal throughout +the solar system. The law, therefore, is stated as +of universal application. "Every particle of matter in +the universe attracts every other particle with a force +varying inversely as the square of the distance between +them, and directly as the product of the masses of the +two particles." And Newton further proved that if a +body, projected in free space and moving with any +velocity, became subject to a central force acting, like +gravitation, inversely as the square of the distance, it +must revolve in an ellipse, or in a closely allied curve. +</p> + +<p> +These curves are what are known as the "<b>conic +sections</b>"—that is, they are the curves found when a +cone is cut across in different directions. Their +relation to each other may be illustrated thus. If we have +a very powerful light emerging from a minute hole, +then, if we place a screen in the path of the beam of +light, and exactly at right angles to its axis, the light +falling on the screen will fill an exact circle. If we +turn the screen so as to be inclined to the axis of the +beam, the circle will lengthen out in one direction, and +will become an ellipse. If we turn the screen still +further, the ellipse will lengthen and lengthen, until at +last, when the screen has become parallel to one of the +edges of the beam of light, the ellipse will only have +one end; the other will be lost. For it is clear that +that edge of the beam of light which is parallel to the +screen can never meet it. The curve now shown on +the screen is called a <b>parabola</b>, and if the screen is turned +further yet, the boundaries of the light falling upon it +become divergent, and we have a fourth curve, the +<b>hyperbola</b>. Bodies moving under the influence of +<span class="pagenum">{<a id="P35"></a>35}</span> +gravitation can move in any of these curves, but only +the circle and ellipse are closed orbits. A particle +moving in a parabola or hyperbola can only make one +approach to its attracting body; after such approach +it continually recedes from it. As the circle and +parabola are only the two extreme forms of an ellipse, the +two foci being at the same point for the circle and at +an infinite distance apart for the parabola, we may +regard all orbits under gravitation as being ellipses of +one form or another. +</p> + +<p> +From his great demonstration of the law of gravitation, +Newton went on to apply it in many directions. +He showed that the Earth could not be truly spherical +in shape, but that there must be a flattening of its +poles. He showed also that the Moon, which is exposed +to the attractions both of the Earth and of the Sun, +and, to a sensible extent, of some of the other planets, +must show irregularities in her motion, which at that +time had not been noticed. The Moon's orbit is +inclined to that of the Earth, cutting its plane in two +opposite points, called the "<b>nodes</b>." It had long been +observed that the position of the nodes travelled round +the ecliptic once in about nineteen years. Newton was +able to show that this was a consequence of the Sun's +attraction upon the Moon. And he further made a +particular application of the principle thus brought out, +for, the Earth not being a true sphere, but flattened +at the poles and bulging at the equator, the equatorial +belt might be regarded as a compact ring of satellites +revolving round the Earth's equator. This, therefore, +would tend to retrograde precisely as the nodes of a +single satellite would, so that the axis of the equatorial +belt of the Earth—in other words, the axis of the +Earth—must revolve round the pole of the ecliptic. +<span class="pagenum">{<a id="P36"></a>36}</span> +Consequently the pole of the heavens appears to move amongst +the stars, and the point where the celestial equator +crosses the equator necessarily moves with it. This is +what we know as the "<b>Precession of the Equinoxes</b>," +and it is from our knowledge of the fact and the amount +of precession that we are able to determine roughly +the date when the first great work of astronomical +observation was accomplished, namely, the grouping of +the stars into constellations by the astronomers of the +prehistoric age. +</p> + +<p> +The publication of Newton's great work, the +<i>Principia</i> (<i>The Mathematical Principles of Natural +Philosophy</i>), in which he developed the Laws of Motion, the +significance of Kepler's Three Planetary Laws, and the +Law of Universal Gravitation, took place in 1687, and +was due to his friend EDMUND HALLEY, to whom he +had confided many of his results. That he was the +means of securing the publication of the <i>Principia</i> is +Halley's highest claim to the gratitude of posterity, +but his own work in the field which Newton had opened +was of great importance. Newton had treated <b>comets</b> +as moving in parabolic orbits, and Halley, collecting all +the observations of comets that were available to him, +worked out the particulars of their orbits on this +assumption, and found that the elements of three were +very closely similar, and that the interval between their +appearances was nearly the same, the comets having +been seen in 1531, 1607, and 1682. On further +consulting old records he found that comets had been +observed in 1456, 1378, and 1301. He concluded that +these were different appearances of the same object, +and predicted that it would be seen again in 1758, or, +according to a later and more careful computation, in +1759. As the time for its return drew near, CLAIRAUT +<span class="pagenum">{<a id="P37"></a>37}</span> +computed with the utmost care the retardation which +would be caused to the comet by the attractions of +Jupiter and Saturn. The comet made its predicted +nearest approach to the Sun on March 13, 1759, just +one month earlier than Clairaut had computed. But +in its next return, in 1835, the computations effected +by PONTÉCOULANT were only two days in error, so +carefully had the comet been followed during its +unseen journey to the confines of the solar system and +back again, during a period of seventy-five years. +Pontécoulant's exploit was outdone at the next return +by Drs. COWELL and CROMMELIN, of Greenwich +Observatory, who not only computed the time of its +perihelion passage—that is to say, its nearest approach to +the Sun—for April 16, 1910, but followed the comet +back in its wanderings during all its returns to the year +240 B.C. Halley's Comet, therefore, was the first comet +that was known to travel in a closed orbit and to return +to the neighbourhood of the Sun. Not a few small or +telescopic comets are now known to be "periodic," but +Halley's is the only one which has made a figure to the +naked eye. Notices of it occur not a few times in +history; it was the comet "like a flaming sword" +which Josephus described as having been seen over +Jerusalem not very long before the destruction by +Titus. It was also the comet seen in the spring of the +year when William the Conqueror invaded England, +and was skilfully used by that leader as an omen of his +coming victory. +</p> + +<p> +The law of gravitation had therefore enabled men +to recognise in Halley's Comet an addition to the +number of the primary bodies in the solar system—the +first addition that had been made since prehistoric +times. On March 13, 1781, Sir WILLIAM HERSCHEL +<span class="pagenum">{<a id="P38"></a>38}</span> +detected a new object, which he at first supposed to +be a comet, but afterwards recognised as a planet far +beyond the orbit of Saturn. This planet, to which the +name of Uranus was finally given, had a mean distance +from the Sun nineteen times that of the Earth, and a +diameter four times as great. This was a second +addition to the solar system, but it was a discovery by +sight, not by deduction. +</p> + +<p> +The first day of the nineteenth century, January 1, +1801, was signalised by the discovery of a small planet +by PIAZZI. The new object was lost for a time, but it +was redetected on December 31 of the same year. +This planet lay between the orbits of Mars and Jupiter—a +region in which many hundreds of other small bodies +have since been found. The first of these "<b>minor planets</b>" +was called Ceres; the next three to be discovered are +known as Pallas, Juno, and Vesta. Beside these four, +two others are of special interest: one, Eros, which +comes nearer the Sun than the orbit of Mars—indeed +at some oppositions it approaches the Earth within +13,000,000 miles, and is therefore, next to the Moon, our +nearest neighbour in space; the other, Achilles, moves +at a distance from the Sun equal to that of Jupiter. +</p> + +<p> +Ceres is much the largest of all the minor planets; +indeed is larger than all the others put together. Yet +the Earth exceeds Ceres 4000 times in volume, and +7000 times in mass, and the entire swarm of minor +planets, all put together, would not equal in total volume +one-fiftieth part of the Moon. +</p> + +<p> +The search for these small bodies rendered it necessary +that much fuller and more accurate maps of the stars +should be made than had hitherto been attempted, +and this had an important bearing on the next great +event in the development of gravitational astronomy. +</p> + +<p> +<span class="pagenum">{<a id="P39"></a>39}</span> +</p> + +<p> +The movements of Uranus soon gave rise to difficulties. +It was found impossible, satisfactorily, to reconcile the +earlier and later observations, and in the tables of +Uranus, published by BOUVARD in 1821, the earlier +observations were rejected. But the discrepancies +between the observed and calculated places for the planet +soon began to reappear and quickly increase, and the +suggestion was made that these discrepancies were due +to an attraction exercised by some planet as yet +unknown. Thus Mrs. Somerville in a little book on the +connection of the physical sciences, published in 1836, +wrote, "Possibly it (that is, Uranus) may be subject to +disturbances from some unseen planet revolving about +the Sun beyond the present boundaries of our system. +If, after the lapse of years, the tables formed from a +combination of numerous observations should still be +inadequate to represent the motions of Uranus, the +discrepancies may reveal the existence, nay, even the +mass and orbit of a body placed for ever beyond the +sphere of vision." In 1843 JOHN C. ADAMS, who had +just graduated as Senior Wrangler at Cambridge, +proceeded to attack the problem of determining the +position, orbit, and mass of the unknown body by which +on this assumption Uranus was disturbed, from the +irregularities evident in the motion of that planet. +The problem was one of extraordinary intricacy, but +by September 1845 Adams had obtained a first solution, +which, he submitted to AIRY, the Astronomer Royal. +As, however, he neglected to reply to some inquiries +made by Airy, no search for the new planet was +instituted in England until the results of a new and +independent worker had been published. The same +problem had been attacked by a well-known and very +gifted French mathematician, U. J. J. LEVERRIER, and +<span class="pagenum">{<a id="P40"></a>40}</span> +in June 1846 he published his position for the unseen +planet, which proved to be in close accord with that +which Adams had furnished to Airy nine months +before. On this Airy stirred up Challis, the Director +of the Cambridge Observatory, which then possessed +the most powerful telescope in England, to search for +the planet, and Challis commenced to make charts, +which included more than 3000 stars, in order to make +sure that the stranger should not escape his net. +Leverrier, on the other hand, communicated his result +to the Berlin Observatory, where they had just received +some of the star charts prepared by Dr. Bremiker in +connection with the search for minor planets. The +Berlin observer, Dr. Galle, had therefore nothing to do +but to compare the stars in the field, upon which he +turned his telescope, with those shown on the chart; a +star not in the chart would probably be the desired +stranger. He found it, therefore, on the very first +evening, September 23, 1846, within less than four +diameters of the Moon of the predicted place. The +same object had been observed by Challis at Cambridge +on August 4 and 12, but he was deferring the reduction +of his observations until he had completed his scrutiny +of the zone, and hence had not recognised it as different +from an ordinary star. +</p> + +<p> +This discovery of the planet now known as Neptune, +which had been disturbing the movement of Uranus, +has rightly been regarded as the most brilliant triumph +of gravitational astronomy. It was the legitimate +crown of that long intellectual struggle which had +commenced more than 2000 years earlier, when the first +Greek astronomers set themselves to unravel the +apparently aimless wanderings of the planets in the assured +faith that they would find them obedient unto law. +<span class="pagenum">{<a id="P41"></a>41}</span> +But of what use was all this effort? What is the good +of astronomy? The question is often asked, but it is +the question of ignorance. The use of astronomy is +the development which it has given to the intellectual +powers of man. Directly the problem of the planetary +motions was first attempted, it became necessary to +initiate mathematical processes in order to deal with it, +and the necessity for the continued development of +mathematics has been felt in the same connection right +down to the present day. When the Greek astronomers +first began their inquiries into the planetary movements +they hoped for no material gain, and they received +none. They laboured; we have entered into their +labours. But the whole of our vast advances in +mechanical and engineering science—advances which +more than anything else differentiate this our present +age from all those which have preceded it—are built +upon our command of mathematics and our knowledge +of the laws of motion—a command and a knowledge +which we owe directly to their persevering attempts to +advance the science of astronomy, and to follow after +knowledge, not for any material rewards which she had +to offer, but for her own sake. +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap04"></a></p> + +<p><span class="pagenum">{<a id="P42"></a>42}</span></p> + +<h3> +CHAPTER IV +</h3> + +<h3> +ASTRONOMICAL MEASUREMENTS +</h3> + +<p> +The old proverb has it that "Science is measurement," +and of none of the sciences is this so true as of the +science of astronomy. Indeed the measurement of +time by observation of the movements of the heavenly +bodies was the beginning of astronomy. The +movement of the Sun gave the day, which was reckoned to +begin either at sunrise or at sunset. The changes of +the Moon gave the month, and in many languages the +root meaning of the word for <i>Moon</i> is "measurer." The +apparent movement of the Sun amongst the stars +gave a yet longer division of time, the year, which +could be determined in a number of different ways, +either from the Sun alone, or from the Sun together +with the stars. A very simple and ancient form of +instrument for measuring this movement of the Sun was +the obelisk, a pillar with a pointed top set up on a level +pavement. Such obelisks were common in Egypt, and +one of the most celebrated, known as Cleopatra's Needle, +now stands on the Thames Embankment. As the Sun +moved in the sky, the shadow of the pillar moved on +the pavement, and midday, or noon, was marked when +the shadow was shortest. The length of the shadow at +noon varied from day to day; it was shortest at +mid-summer, and longest at midwinter, <i>i.e.</i> at the summer +and winter solstices. Twice in the year the shadow of +the pillar pointed due west at sunrise, and due east at +<span class="pagenum">{<a id="P43"></a>43}</span> +sunset—that is to say, the shadow at the beginning of +the day was in the same straight line as at its end. +These two days marked the two equinoxes of spring +and autumn. +</p> + +<p> +The obelisk was a simple means of measuring the +height and position of the Sun, but it had its +drawbacks. The length of the shadow and its direction did +not vary by equal amounts in equal times, and if the +pavement upon which the shadow fell was divided by +marks corresponding to equal intervals of time for one +day of the year, the marks did not serve for all other +days. +</p> + +<p> +But if for the pillar a triangular wall was substituted—a +wall rising from the pavement at the south and sloping +up towards the north at such an angle that it seemed +to point to the invisible pivot of the heavens, round +which all the stars appeared to revolve—then the shadow +of the wall moved on the pavement in the same manner +every day, and the pavement if marked to show the +hours for one day would show them for any day. The +sundials still often found in the gardens of country +houses or in churchyards are miniatures of such an +instrument. +</p> + +<p> +But the Greek astronomers devised other and better +methods for determining the positions of the heavenly +bodies. Obelisks or dials were of use only with the +Sun and Moon which cast shadows. To determine the +position of a star, "sights" like those of a rifle were +employed, and these were fixed to circles which were +carefully divided, generally into 360 "degrees." As +there are 365 days in a year, and as the Sun makes a +complete circuit of the Zodiac in this time, it moves +very nearly a degree in a day. The twelve Signs of +the Zodiac are therefore each 30° in length, and each +<span class="pagenum">{<a id="P44"></a>44}</span> +takes on the average a double-hour to rise or set. +While the Sun and Moon are each about half a degree +in diameter, <i>i.e.</i> about one-sixtieth of the length of +a Sign, and therefore take a double-minute to rise or +set. Each degree of a circle is therefore divided into +60 minutes, and each minute may be divided into 60 +seconds. +</p> + +<p> +As the Sun or Moon are each about half a degree, or, +more exactly, 32 minutes in diameter, it is clear that, +so long as astronomical observations were made by the +unaided sight, a minute of arc (written 1') was the +smallest division of the circle that could be used. A +cord or wire can indeed be detected when seen +projected against a moderately bright background if its +thickness is a second of arc (written 1")—a sixtieth of +a minute—but the wire is merely perceived, not +properly defined. +</p> + +<p> +Tycho Brahe had achieved the utmost that could be +done by the naked eye, and it was the certainty that he +could not have made a mistake in an observation in +the place of the planet Mars amounting to as much as +8 minutes of arc—that is to say, of a quarter the +apparent diameter of the Moon—that made Kepler finally +give up all attempts to explain the planetary +movements on the doctrine of circular orbits and to try +movements in an ellipse. But a contemporary of +Kepler, as gifted as he was himself, but in a different +direction, was the means of increasing the observing +power of the astronomer. GALILEO GALILEI (1564-1642), +of a noble Florentine family, was appointed +Lecturer in Mathematics at the University of Pisa. +Here he soon distinguished himself by his originality of +thought, and the ingenuity and decisiveness of his +experiments. Up to that time it had been taught that of +<span class="pagenum">{<a id="P45"></a>45}</span> +two bodies the heavier would fall to the ground more +quickly than the lighter. Galileo let fall a 100-lb. +weight and a 1-lb. weight from the top of the Leaning +Tower, and both weights reached the pavement together. +By this and other ingenious experiments he laid a firm +foundation for the science of mechanics, and he +discovered the laws of motion which Newton afterwards +formulated. He heard that an instrument had been +invented in Holland which seemed to bring distant +objects nearer, and, having himself a considerable +knowledge of optics, it was not long before he made himself +a little telescope. He fixed two spectacle glasses, one +for long and one for short sight, in a little old +organ-pipe, and thus made for himself a telescope which +magnified three times. Before long he had made +another which magnified thirty times, and, turning it +towards the heavenly bodies, he discovered dark moving +spots upon the Sun, mountains and valleys on the +Moon, and four small satellites revolving round Jupiter. +He also perceived that Venus showed "<b>phases</b>"—that is +to say, she changed her apparent shape just as the +Moon does—and he found the Milky Way to be +composed of an immense number of small stars. These +discoveries were made in the years 1609-11. +</p> + +<p> +A telescope consists in principle of two parts—an +<b>object-glass</b>, to form an image of the distant object, +and an <b>eye-piece</b>, to magnify it. The rays of light from +the heavenly body fall on the object-glass, and are so +bent out of their course by it as to be brought together +in a point called the focus. The "light-gathering +power" of the telescope, therefore, depends upon the +size of the object-glass, and is proportional to its area. +But the size of the image depends upon the focal length +of the telescope, <i>i.e.</i> upon the distance that the focus +<span class="pagenum">{<a id="P46"></a>46}</span> +is from the object-glass. Thus a small disc, an inch in +diameter—such as a halfpenny—will exactly cover the +full Moon if held up nine feet away from the eye; and +necessarily the image of the full Moon made by an +object-glass of nine-feet focus will be an inch in diameter. +The eye-piece is a magnifying-glass or small microscope +applied to this image, and by it the image can be +magnified to any desired amount which the quality of +the object-glass and the steadiness of the atmosphere +may permit. +</p> + +<p> +This little image of the Moon, planet, or group of stars +lent itself to measurement. A young English gentleman, +GASCOIGNE, who afterwards fell at the Battle of +Marston Moor, devised the "micrometer" for this +purpose. The micrometer usually has two frames, each +carrying one or more very thin threads—usually spider's +threads—and the frames can be moved by very fine +screws, the number of turns or parts of a turn of each +screw being read off on suitable scales. By placing one +thread on the image of one star, and the other on the +image of another, the apparent separation of the two +can be readily and precisely measured. +</p> + +<p> +Within the last thirty years photography has +immensely increased the ease with which astronomical +measurements can be made. The sensitive photographic +plate is placed in the focus of the telescope, and the +light of Sun, Moon, or stars, according to the object to +which the telescope is directed, makes a permanent +impression on the plate. Thus a picture is obtained, +which can be examined and measured in detail at any +convenient time afterwards; a portion of the heavens +is, as it were, brought actually down to the astronomer's +study. +</p> + +<p> +It was long before this great advance was effected. +<span class="pagenum">{<a id="P47"></a>47}</span> +The first telescopes were very imperfect, for the rays of +different colour proceeding from any planet or star +came to different foci, so that the image was coloured, +diffused, and ill-defined. The first method by which +this difficulty was dealt with was by making telescopes +of enormously long focal length; 80, 100, or 150 feet +were not uncommon, but these were at once +cumbersome and unsteady. Sir Isaac Newton therefore +discarded the use of object-glasses, and used curved +mirrors in order to form the image in the focus, and +succeeded in making two telescopes on this principle of +reflection. Others followed in the same direction, and +a century later Sir WILLIAM HERSCHEL was most +skilful and successful in making "<b>reflectors</b>," his largest +being 40 feet in focal length, and thus giving an image +of the Moon in its focus of nearly 4-½ inches diameter. +</p> + +<p> +But in 1729 CHESTER MOOR HALL found that by +combining two suitable lenses together in the object-glass +he could get over most of the colour difficulty, +and in 1758 the optician DOLLOND began to make +object-glasses that were almost free from the colour +defect. From that time onward the manufacture of +"<b>refractors</b>," as object-glass telescopes are called, has +improved; the glass has been made more transparent +and more perfect in quality, and larger in size, and the +figure of the lens improved. The largest refractor now +in use is that of the Yerkes Observatory, Wisconsin, +U.S.A., and is 40 inches in aperture, with a focal length +of 65 feet, so that the image of the Moon in its focus +has a diameter of more than 7 inches. At present this +seems to mark the limit of size for refractors, and the +difficulty of getting good enough glass for so large a +lens is very great indeed. Reflectors have therefore +come again into favour, as mirrors can be made larger +<span class="pagenum">{<a id="P48"></a>48}</span> +than any object-glass. Thus Lord Rosse's great +telescope was 6 feet in diameter; and the most powerful +telescope now in action is the great 5-foot mirror of the +Mt. Wilson Observatory, California, with a focal length, +as sometimes used, of 150 feet. Thus its light-gathering +power is about 60,000 times that of the unaided eye, +and the full Moon in its focus is 17 inches in diameter; +such is the enormous increase to man's power of sight, +and consequently to his power of learning about the +heavenly bodies, which the development of the telescope +has afforded to him. +</p> + +<p> +The measurement of time was the first purpose for +which men watched the heavenly bodies; a second +purpose was the measurement of the size of the Earth. +If at one place a star was observed to pass exactly +overhead, and if at another, due south of it, the same star +was observed to pass the meridian one degree north of +the zenith, then by measuring the distance between the +two places the circumference of the whole Earth would +be known, for it would be 360 times that amount. In +this way the size of the Earth was roughly ascertained +2000 years before the invention of the telescope. But +with the telescope measures of much greater precision +could be made, and hence far more difficult problems +could be attacked. +</p> + +<p> +One great practical problem was that of finding out +the position of a ship when out of sight of land. The +ancient Phoenician and Greek navigators had mostly +confined themselves to coasting voyages along the shores +of the Mediterranean Sea, and therefore the quick +recognition of landmarks was the first requisite for a good +sailor. But when, in 1492, Columbus had brought a +new continent to light, and long voyages were freely +taken across the great oceans, it became an urgent +<span class="pagenum">{<a id="P49"></a>49}</span> +necessity for the navigator to find out his position when +he had been out of sight of any landmark for weeks. +</p> + +<p> +This necessity was especially felt by the nations of +Western Europe, the countries facing the Atlantic with +the New World on its far-distant other shore. Spain, +France, England, and Holland, all were eager +competitors for a grasp on the new lands, and therefore +were earnest in seeking a solution of the problem of +navigation. +</p> + +<p> +The latitude of the ship could be found out by +observing the height of the Sun at noon, or of the Pole +Star at night, or in several other ways. But the +longitude was more difficult. As the Earth turns on its +axis, different portions of its surface are brought in +succession under the Sun, and if we take the moment +when the Sun is on the meridian of any place as its +noon, as twelve o'clock for that place, then the difference +of longitude between any two places is essentially +the difference in their local times. +</p> + +<p> +It was possible for the sailor to find out when it was +local noon for him, but how could he possibly find out +what time it was at that moment at the port from +which he had sailed, perhaps several weeks before? +</p> + +<p> +The Moon and stars supplied eventually the means +for giving this information. For the Moon moves +amongst the stars, as the hand of a clock moves +amongst the figures of a dial, and it became possible +at length to predict for long in advance exactly where +amongst the stars the Moon would be, for any given +time, of any selected place. +</p> + +<p> +When this method was first suggested, however, +neither the motion of the Moon nor the places of the +principal stars were known with sufficient accuracy, and +it was to remedy this defect, and put navigation upon +<span class="pagenum">{<a id="P50"></a>50}</span> +a sound basis, that CHARLES II. founded Greenwich +Observatory in the year 1675, and appointed +FLAMSTEED the first Astronomer Royal. In the year 1767 +MASKELYNE, the fifth Astronomer Royal, brought out +the first volume of the <i>Nautical Almanac</i>, in which the +positions of the Moon relative to certain stars were +given for regular intervals of Greenwich time. Much +about the same period the problem was solved in +another way by the invention of the chronometer, by +JOHN HARRISON, a Yorkshire carpenter. The <b>chronometer</b> +was a large watch, so constructed that its rate +was not greatly altered by heat or cold, so that the +navigator had Greenwich time with him wherever he +went. +</p> + +<p> +The new method in the hands of CAPTAIN COOK and +other great navigators led to a rapid development of +navigation and the discovery of Australia and New +Zealand, and a number of islands in the Pacific. The +building up of the vast oceanic commerce of Great +Britain and of her great colonial empire, both in North +America and in the Southern Oceans, has arisen out +of the work of the Royal Observatory, Greenwich, and +has had a real and intimate connection with it. +</p> + +<p> +To observe the motions of the Moon, Sun, and planets, +and to determine with the greatest possible precision +the places of the stars have been the programme of +Greenwich Observatory from its foundation to the +present time. Other great national observatories have +been Copenhagen, founded in 1637; Paris, in 1667; +Berlin, in 1700; St. Petersburg, in 1725, superseded by +that of Pulkowa, in 1839; and Washington, in 1842; +while not a few of the great universities have also +efficient observatories connected with them. +</p> + +<p> +Of the directly practical results of astronomy, the +<span class="pagenum">{<a id="P51"></a>51}</span> +promotion of navigation stands in the first rank. But +the science has never been limited to merely utilitarian +inquiries, and the problem of measuring celestial +distances has followed on inevitably from the measurement +of the Earth. +</p> + +<p> +The first distance to be attacked was that of the +nearest companion to the Earth, <i>i.e.</i> the Moon. It +often happens on our own planet that it is required to +find the distance of an object beyond our reach. Thus +a general on the march may come to a river and need +to know exactly how broad it is, that he may prepare +the means for bridging it. Such problems are usually +solved on the following principle. Let A be the distant +object. Then if the direction of A be observed from +each of two stations, B and C, and the distance of B +from C be measured, it is possible to calculate the +distances of A from B and from C. The application of +this principle to the measurement of the Moon's +distance was made by the establishment of an observatory +at the Cape of Good Hope, to co-operate with that of +Greenwich. It is, of course, not possible to see +Greenwich Observatory from the Cape, or vice versa, but the +stars, being at an almost infinite distance, lie in the +same direction from both observatories. What is +required then is to measure the apparent distance of +the Moon from the same stars as seen from Greenwich +and as seen from the Cape, and, the distance apart of +the two observatories being known, the distance of the +Moon can be calculated. +</p> + +<p> +This was a comparatively easy problem. The next +step in celestial measurement was far harder; it was +to find the distance of the Sun. The Sun is 400 times +as far off as the Moon, and therefore it seems to be +practically in the same direction as seen from each of +<span class="pagenum">{<a id="P52"></a>52}</span> +the two observatories, and, being so bright, stars cannot +be seen near it in the telescope. But by carefully +watching the apparent movements of the planets their +<i>relative</i> distances from the Sun can be ascertained, and +were known long before it was thought possible that +we should ever know their real distances. Thus Venus +never appears to travel more than 47° 15' from the +Sun. This means that her distance from the Sun is a +little more than seven-tenths of that of the Earth. +If, therefore, the distance of one planet from the +Sun can be measured, or the distance of one planet +from the Earth, the actual distances of all the planets +will follow. We know the proportions of the parts of +the solar system, and, if we can fix the scale of one of +the parts, we fix the scale of all. +</p> + +<p> +It has been found possible to determine the distance +of Mars, of several of the "minor planets," and +especially of Eros, a very small minor planet that sometimes +comes within 13,000,000 miles of the Earth, or seven +times nearer to us than is the Sun. +</p> + +<p> +From the measures of Eros, we have learned that the +Sun is separated from us by very nearly 93,000,000 +miles—an unimaginable distance. Perhaps the nearest +way of getting some conception of this vast interval is +by remembering that there are only 31,556,926 seconds +of time in a year. If, therefore, an express train, +travelling 60 miles an hour—a mile a minute—set out +for the Sun, and travelled day and night without cease, +it would take more than 180 years to accomplish the +journey. +</p> + +<p> +But this astronomical measure has led on to one +more daring still. The earth is on one side of the Sun +in January, on the other in July. At these two dates, +therefore, we are occupying stations 186,000,000 miles +<span class="pagenum">{<a id="P53"></a>53}</span> +apart, and can ascertain the apparent difference in +direction of the stars as viewed from the two points +But the astonishing result is that this enormous change +in the position of the Earth makes not the slightest +observable difference in the position of most of the +stars. A few, a very few, do show a very slight +difference. The nearest star to us is about 280,000 times as +far from us as the Sun; this is Alpha Centauri, the +brightest star in the constellation of the Centaur and +the third brightest star in the sky. Sirius, the brightest +star, is twice this distance. Some forty or fifty stars +have had their distances roughly determined; but the +stars in general far transcend all our attempts to plumb +their distances. But, from certain indirect hints, it is +generally supposed that the mass of stars in the Milky +Way are something like 300,000,000 times as far from +us as we are from our Sun. +</p> + +<p> +Thus far, then, astronomy has led us in the direction +or measurement. It has enabled us to measure the +size of the Earth upon which we live, and to find out +the position of a ship in the midst of the trackless ocean. +It has also enabled us to cast a sounding-line into +space, to show how remote and solitary the earth moves +through the void, and to what unimaginable lengths +the great stellar universe, of which it forms a secluded +atom, stretches out towards infinity. +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap05"></a></p> + +<p><span class="pagenum">{<a id="P54"></a>54}</span></p> + +<h3> +CHAPTER V +</h3> + +<h3> +THE MEMBERS OF THE SOLAR SYSTEM +</h3> + +<p> +Astronomical measurement has not only given us the +distances of the various planets from the Sun; it has +also furnished us, as in the annexed table, with their +real diameters, and, as a consequence of the law of +gravitation, with their densities and weights, and the +force of gravity at their surfaces. And these numerical +details are of the first importance in directing us as to +the inferences that we ought to draw as to their present +physical conditions. +</p> + +<p> +The theory of Copernicus deprived the Earth of its +special position as the immovable centre of the +universe, but raised it to the rank of a planet. It is +therefore a heavenly body, yet needs no telescope to bring +it within our ken; bad weather does not hide it from +us, but rather shows it to us under new conditions. +We find it to be a globe of land and water, covered by +an atmosphere in which float changing clouds; we have +mapped it, and we find that the land and water are +always there, but their relations are not quite fixed; +there is give and take between them. We have found +of what elements the land and water consist, and how +these elements combine with each other or dissociate. +In a word, the Earth is the heavenly body that we know +the best, and with it we must compare and contrast all +the others. +</p> + +<p> +Before the invention of the telescope there were but +<span class="pagenum">{<a id="P55"></a>55}</span> +two other heavenly bodies—the Sun and the Moon—that +appeared as orbs showing visible discs, and even +in their cases nothing could be satisfactorily made out +as to their conditions. Now each of the five planets +known to the ancients reveals to us in the telescope a +measurable disc, and we can detect significant details +on their surfaces. +</p> + +<p> +THE MOON is the one object in the heavens which +does not disappoint a novice when he first sees it in the +telescope. Every detail is hard, clear-cut, and sharp; +it is manifest that we are looking at a globe, a very +rough globe, with hills and mountains, plains and valleys, +the whole in such distinct relief that it seems as if it +might be touched. No clouds ever conceal its details, +no mist ever softens its outlines; there are no +half-lights, its shadows are dead black, its high lights are +molten silver. Certain changes of illumination go on +with the advancing age of the Moon, as the crescent +broadens out to the half, the half to the full, and the +full, in its turn, wanes away; but the lunar day is +nearly thirty times as long as that of the Earth, and +these changes proceed but slowly. +</p> + +<p> +The full Moon, as seen by the naked eye, shows several +vague dark spots, which most people agree to fancy as +like the eyes, nose, and mouth of a broad, sorrowful +face. The ordinary astronomical telescope inverts the +image, so the "eyes" of the Moon are seen in the lower +part of the field of the telescope as a series of dusky +plains stretching right across the disc. But in the +upper part, near the left-hand corner of the underlip, +there is a bright, round spot, from which a number of +bright streaks radiate—suggesting a peeled orange with +its stalk, and the lines marking the sections radiating +from it. This bright spot has been called after the great +<span class="pagenum">{<a id="P56"></a>56}</span> +</p> + +<p><br /></p> + +<pre> + Mean distance from Sun. Period Velocity + Class. Name. Earth's In millions of revolution. in orbit. Eccentricity. + distance of miles. In years. Miles per + = 1. sec. + + Terrestrial Mercury 0.387 36.0 0.24 29.7 0.2056 + Planets Venus 0.723 67.2 0.62 21.9 0.0068 + Earth 1.000 92.9 1.00 18.5 0.0168 + Mars 1.524 141.5 1.88 15.0 0.0933 + + Minor Eros 1.458 135.5 1.76 15.5 0.2228 + Planets Ceres 2.767 257.1 4.60 11.1 0.0763 + Achilles 5.253 488.0 12.04 8.1 0.0509 + + Major Jupiter 5.203 483.3 11.86 8.1 0.0483 + Planets Saturn 9.539 886.6 29.46 6.0 0.0561 + Uranus 19.183 1781.9 84.02 4.2 0.0463 + Neptune 30.055 2791.6 164.78 3.4 0.0090 +</pre> + +<p><br /></p> + +<p> +<span class="pagenum">{<a id="P57"></a>57}</span> +</p> + +<p><br /></p> + +<pre> + Mean diameter. Surface. Volume. Mass. + Name. Symbol. In miles. [Earth]=1. [Earth]=1. [Earth]=1. [Earth]=1. + + Sun [Sun] 866400 109.422 11973. 1310130. 332000. + Moon [Moon] 2163 0.273 0.075 0.02 0.012 + + Mercury [Mercury] 3030 0.383 0.147 0.06 0.048 + Venus [Venus] 7700 0.972 0.945 0.92 0.820 + Earth [Earth] 7918 1.000 1.000 1.00 1.000 + Mars [Mars] 4230 0.534 0.285 0.15 0.107 + + Jupiter [Jupiter] 86500 10.924 119.3 1304. 317.7 + Saturn [Saturn] 73000 9.219 85.0 783. 94.8 + Uranus [Uranus] 31900 4.029 16.2 65. 14.6 + Neptune [Neptune] 34800 4.395 19.3 85. 17.0 +</pre> + +<p><br /></p> + +<p> +<span class="pagenum">{<a id="P58"></a>58}</span> +</p> + +<p><br /></p> + +<pre> + Light + Gravity. and heat Albedo; + Density. Fall in received <i>i.e.</i> re- + [Earth] Water [Earth] feet per from Sun. Time of rotation flecting + Name. =1. =1. =1. sec. [Earth]=1. on axis. power. + + d. h. m. + Sun 0.25 1.39 27.65 444.60 ... 25 4 48 ± ... + Moon 0.61 3.39 0.17 2.73 1.00 27 7 43 0.17 + + d. h. m. s. + Mercury 0.85 4.72 0.43 6.91 6.67 88 (?) 0.14 + Venus 0.89 4.94 0.82 13.19 1.91 23 21 23 (?) 0.76 + Earth 1.00 5.55 1.00 16.08 1.00 23 56 4 0.50 (?) + Mars 0.71 3.92 0.38 6.11 0.43 24 37 23 0.22 + + h. m. + Jupiter 0.24 1.32 2.65 42.61 0.037 9 55 ± 0.62 + Saturn 0.13 0.72 1.18 18.97 0.011 10 14 ± 0.72 + Uranus 0.22 1.22 0.90 14.47 0.003 9 30 (?) 0.60 + Neptune 0.20 1.11 0.89 14.31 0.001 (?) 0.52 +</pre> + +<p><br /></p> + +<p class="noindent"> +<span class="pagenum">{<a id="P59"></a>59}</span> +Danish astronomer, "Tycho," and is one of the most +conspicuous objects of the full Moon. +</p> + +<p> +The contrasts of the Moon are much more +pronounced when she is only partly lit up. Then the +mountains and valleys stand out in the strongest relief, +and it becomes clear that the general type of formation +on the Moon is that of rings—rings of every conceivable +size, from the smallest point that the telescope can +detect up to some of the great dusky plains +themselves, hundreds of miles in diameter. These rings are +so numerous that Galileo described the Moon as +looking as full of "eyes" as a peacock's tail. +</p> + +<p> +The "right eye" of the moonface, as we see it in the +sky, is formed by a vast dusky plain, nearly as large +as France and Germany put together, to which has +been given the name of the "Sea of Rains" (<i>Mare +Imbrium</i>), and just below this (as seen in the +telescope) is one of the most perfect and beautiful of all +the lunar rings—a great ring-plain, 56 miles in diameter, +called after the thinker who revolutionised men's ideas +of the solar system, "Copernicus." "Copernicus," like +"Tycho," is the centre of a set of bright streaks; +and a neighbouring but smaller ring, bearing the +great name of "Kepler," stands in a like relation to +another set. +</p> + +<p> +The most elevated region of the Moon is immediately +in the neighbourhood of the great "stalk of the orange," +"Tycho." Here the rings are crowded together as +closely as they can be packed; more closely in many +places, for they intrude upon and overlap each other +in the most intricate manner. A long chain of fine +rings stretches from this disturbed region nearly to +the centre of the disc, where the great Alexandrian +astronomer is commemorated by a vast walled plain, +<span class="pagenum">{<a id="P60"></a>60}</span> +considerably larger than the whole of Wales, and known +as "Ptolemæus." +</p> + +<p> +The distinctness of the lunar features shows at once +that the Moon is in an altogether different condition +from that of the Earth. Here the sky is continually +being hidden by cloud, and hence the details of the +surface of the Earth as viewed from any other planet +must often be invisible, and even when actual cloud is +absent there is a more permanent veil of dust, which +must greatly soften and confuse terrestrial outlines. +The clearness, therefore, with which we perceive the +lunar formations proves that there is little or no +atmosphere there. Nor is there any sign upon +it of water, either as seas or lakes or running +streams. +</p> + +<p> +Yet the Moon shows clearly that in the past it has +gone through great and violent changes. The +gradation is so complete from the little craterlets, which +resemble closely, in form and size, volcanic craters on +the Earth, up to the great ring-plains, like "Copernicus" +or "Tycho," or formations larger still, that it +seems natural to infer not only that the smaller craters +were formed by volcanic eruption, like the similar +objects with which we are acquainted on our own Earth, +but that the others, despite their greater sizes, had a +like origin. In consequence of the feebler force of +gravity on the Moon, the same explosive force there +would carry the material of an eruption much further +than on the Earth. +</p> + +<p> +The darker, low-lying districts of the Moon give +token of changes of a different order. It is manifest +that the material of which the floors of these plains is +composed has invaded, broken down, and almost +submerged many of the ring-formations. Sometimes half +<span class="pagenum">{<a id="P61"></a>61}</span> +of a ring has been washed away; sometimes just the +outline of a ring can still be traced upon the floor of +the sea; sometimes only a slight breach has been +made in the wall. So it is clear that the Moon was +once richer in the great crater-like formations than it +is to-day, but a lava-flood has overflowed at least +one-third of its area. More recent still are the bright +streaks, or rays, which radiate in all directions from +"Tycho," and from some of the other ring-plains. +</p> + +<p> +It is evident from these different types of structure +on the Moon, and from the relations which they bear to +each other, that the lunar surface has passed through +several successive stages, and that its changes tended, +on the whole, to diminish in violence as time went on; +the minute crater pits with which the surface is stippled +having been probably the last to form. +</p> + +<p> +But the 300 years during which the Moon has been +watched with the telescope have afforded no trace of +any continuance of these changes. She has had a +stormy and fiery past; but nothing like the events of +those bygone ages disturbs her serenity to-day. +</p> + +<p> +And yet we must believe that change does take place +on the Moon even now, because during the 354 hours +of its long day the Sun beats down with full force on +the unprotected surface, and during the equally long +night that surface is exposed to the cold of outer space. +Every part of the surface must be exposed in turn to +an extreme range of temperature, and must be cracked, +torn, and riven by alternate expansion and contraction. +Apart from this slow, wearing process, and a very few +rather doubtful cases in which a minute alteration of +some surface detail has been suspected, our sister planet, +the Moon, shows herself as changeless and inert, +without any appreciable trace of air or water or any sign +<span class="pagenum">{<a id="P62"></a>62}</span> +of life—a dead world, with all its changes and activities +in the past. +</p> + +<p> +MARS, after the Moon, is the planet whose surface we +can study to best advantage. Its orbit lies outside +that of the Earth, so that when it is nearest to us it +turns the same side to both the Sun and Earth, and we +see it fully illuminated. Mercury and Venus, on the +contrary, when nearest us are between us and the +Sun, and turn their dark sides to us. When fully +illuminated they are at their greatest distance, and +appear very small, and, being near the Sun, are observed +with difficulty. These three are intermediate in size +between the Moon and the Earth. +</p> + +<p> +In early telescopic days it was seen that Mars was +an orange-coloured globe with certain dusky markings +upon it, and that these markings slowly changed their +place—that, in short, it was a world rotating upon its +axis, and in a period not very different from that of +the Earth. The rotation period of Mars has indeed +been fixed to the one-hundredth part of a second of +time; it is 24 h. 37 m. 22.67 s. And this has been +possible because some of the dusky spots observed in +the seventeenth century can be identified now in the +twentieth. Some of the markings on Mars, like our +own continents and seas, and like the craters on the +Moon, are permanent features; and many charts of +the planet have been constructed. +</p> + +<p> +Other markings are variable. Since the planet +rotates on its axis, the positions of its poles and equator +are known, its equator being inclined to its orbit at an +angle of 24° 50', while the angle in the case of the +Earth is 23° 27'. The times when its seasons begin +and end are therefore known; and it is found that +the spring of its northern hemisphere lasts 199 of our +<span class="pagenum">{<a id="P63"></a>63}</span> +days, the summer 183, the autumn 147, and the winter +158. Round the pole in winter a broad white cap +forms, which begins to shrink as spring comes on, and +may entirely disappear in summer. No corresponding +changes have been observed on the Moon, but it is +easy to find an analogy to them on the Earth. Round +both our poles a great cap of ice and snow is spread—a +cap which increases in size as winter comes on, and +diminishes with the advance of summer—and it seems +a reasonable inference to suppose that the white polar +caps of Mars are, like our own, composed of ice and +snow. +</p> + +<p> +From time to time indications have been observed +of the presence on Mars of a certain amount of cloud. +Familiar dark markings have, for a short time, been +interrupted, or been entirely hidden, by white bands, +and have recovered their ordinary appearance later. +With rotation on its axis and succession of seasons, +with atmosphere and cloud, with land and water, with +ice and snow, Mars would seem to be a world very +similar to our own. +</p> + +<p> +This was the general opinion up to the year 1877, +when SCHIAPARELLI announced that he had discovered +a number of very narrow, straight, dark lines on the +planet—lines to which he gave the name of "canali"—that +is, "channels." This word was unfortunately +rendered into English by the word "<b>canals</b>," and, as a +canal means a waterway artificially made, this +mistranslation gave the idea that Mars was inhabited by +intelligent beings, who had dug out the surface of the +planet into a network of canals of stupendous length +and breadth. +</p> + +<p> +The chief advocate of this theory is LOWELL, an +American observer, who has given very great attention +<span class="pagenum">{<a id="P64"></a>64}</span> +to the study of the planet during the last seventeen +years. His argument is that the straight lines, the +canals, which he sees on the planet, and the round +dots, the "<b>oases</b>," which he finds at their intersections, +form a system so obviously <i>un</i>natural, that it must be +the work of design—of intelligent beings. The canals +are to him absolutely regular and straight, like lines +drawn with ruler and pen-and-ink, and the oases are +exactly round. But, on the one hand, the best +observers, armed with the most powerful telescopes, have +often been able to perceive that markings were really +full of irregular detail, which Lowell has represented +as mere hard straight lines and circular dots, and, on +the other hand, the straight line and the round dot are +the two geometric forms which all very minute objects +must approach in appearance. That we cannot see +irregularities in very small and distant objects is no +proof at all that irregularities do not exist in them, +and it has often happened that a marking which +appeared a typical "canal" when Mars was at a great +distance lost that appearance when the planet was +nearer. +</p> + +<p> +Astronomers, therefore, are almost unanimous that +there is no reason for supposing that any of the details +that we see on the surface of Mars are artificial in their +origin. And indeed the numerical facts that we know +about the planet render it almost impossible that there +should be any life upon it. +</p> + +<p> +If we turn to the table, we see that in size, volume, +density, and force of gravity at its surface, Mars lies +between the Moon and the Earth, but is nearer the +Moon. This has an important bearing as to the +question of the planet's atmosphere. On the Earth we pass +through half the atmosphere by ascending a mountain +<span class="pagenum">{<a id="P65"></a>65}</span> +that is three and a third miles in height; on Mars we +should have to ascend nearly nine miles. If the +atmospheric pressure at the surface of Mars were as great +as it is at the surface of the Earth, his atmosphere +would be far deeper than ours and would veil the planet +more effectively. But we see the surface of Mars with +remarkable distinctness, almost as clearly, when its +greater distance is allowed for, as we see the Moon. +It is therefore accepted that the atmospheric pressure +at the surface of Mars must be very slight, probably +much less than at the top of our very highest mountains, +where there is eternal snow, and life is completely +absent. +</p> + +<p> +But Mars compares badly with the Earth in another +respect. It receives less light and heat from the Sun +in the proportion of three to seven. This we may +express by saying that Mars, on the whole, is almost +as much worse off than the Earth as a point on the +Arctic Circle is worse off than a point on the Equator. +The mean temperature of the Earth is taken as about +60° of the Fahrenheit thermometer (say, 15° Cent.); the +mean temperature of Mars must certainly be considerably +below freezing-point, probably near 0° F. Here +on our Earth the boiling-point of water is 212°, and, +since the mean temperature is 60° and water freezes +at 32°, it is normally in the liquid state. On Mars it +must normally be in the solid state—ice, snow, or +frost, or the like. But with so rare an atmosphere +water will boil at a low temperature, and it is not +impossible that under the direct rays of the Sun—that is +to say, at midday of the torrid zone of Mars—ice may +not only melt, but water boil by day, condensing and +freezing again during the night. NEWCOMB, the +foremost astronomer of his day, concluded "that during +<span class="pagenum">{<a id="P66"></a>66}</span> +the night of Mars, even in the equatorial regions, the +surface of the planet probably falls to a lower +temperature than any we ever experienced on our globe. +If any water exists, it must not only be frozen, but the +temperature of the ice must be far below the freezing +point.... The most careful calculation shows that +if there are any considerable bodies of water on our +neighbouring planet, they exist in the form of ice, and +can never be liquid to a depth of more than one or two +inches, and that only within the torrid zone and during +a few hours each day." With regard to the snow caps +of Mars, Newcomb thought it not possible that any +considerable fall of snow could ever take place. He +regarded the white caps as simply due to a thin deposit +of hoar frost, and it cannot be deemed wonderful that +such should gradually disappear, when it is remembered +that each of the two poles of Mars is in turn presented +to the Sun for more than 300 consecutive days. +Newcomb's conclusion was: "Thus we have a kind of Martian +meteorological changes, very slight indeed, and +seemingly very different from those of our Earth, but yet +following similar lines on their small scale. For snowfall +substitute frostfall; instead of (the barometer reading) +feet or inches say fractions of a millimetre, and instead +of storms or wind substitute little motions of an air +thinner than that on the top of the Himalayas, and we +shall have a general description of Martian meteorology." +</p> + +<p> +We conclude, then, that Mars is not so inert a world +as the Moon, but, though some slight changes of climate +or weather take place upon it, it is quite unfitted for +the nourishment and development of the different forms +of organic life. +</p> + +<p> +Of MERCURY we know very little. It is smaller than +Mars but larger than the Moon, but it differs from them +<span class="pagenum">{<a id="P67"></a>67}</span> +both in that it is much nearer the Sun, and receives, +therefore, many times the light and heat, surface for +surface. We should expect, therefore, that water on +Mercury would exist in the gaseous state instead of in +the solid state as on Mars. The little planet reflects +the sunlight only feebly, and shows no evidence of +cloud. A few markings have been made out on its +surface, and the best observers agree that it appears to +turn the same face always to the Sun. This would +imply that the one hemisphere is in perpetual +darkness and cold, the other, exposed to an unimaginable +fiery heat. +</p> + +<p> +VENUS is nearly of the same size as the Earth, and +the conditions as to the arrangement of its atmosphere, +the force of gravity at its surface, must be nearly the +same as on our own world. But we know almost +nothing of the details of its surface; the planet is very +bright, reflecting fully seven-tenths of the sunlight that +falls upon it. It would seem that, in general, we see +nothing of the actual details of the planet, but only +the upper surface of a very cloudy atmosphere. Owing +to the fact that Venus shows no fixed definite marking +that we can watch, it is still a matter of controversy as +to the time in which it rotates upon its axis. Schiaparelli +and some other observers consider that it rotates +in the same time as it revolves round the Sun. Others +believe that it rotates in a little less than twenty-four +hours. If this be so, and there is any body in the solar +system other than the Earth, which is adapted to be the +home of life, then the planet Venus is that one. +</p> + +<p> +THE SUN, like the Moon, presents a visible surface to +the naked eye, but one that shows no details. In the +telescope the contrast between it and the Moon is very +great, and still greater is the contrast which is brought +<span class="pagenum">{<a id="P68"></a>68}</span> +out by the measurements of its size, volume, and weight. +But the really significant difference is that the Sun is +a body giving out light and heat, not merely reflecting +them. Without doubt this last difference is connected +most closely with the difference in size. The Moon is +cold, dead, unchanging, because it is a small world; +the Sun is bright, fervent, and undergoes the most +violent change, because it is an exceedingly large world. +</p> + +<p> +The two bodies—the Sun and Moon—appear to the eye +as being about the same size, but since the Sun is 400 +times as far off as the Moon it must be 400 times the +diameter. That means that it has 400 times 400, or +160,000 times the surface and 400 times 400 times 400, +or 64,000,000 times the volume. The Sun and Moon, +therefore, stand at the very extremes of the scale. +</p> + +<p> +The heat of the Sun is so great that there is some +difficulty in observing it in the telescope. It is not +sufficient to use a dark glass in order to protect the eye, +unless the telescope be quite a small one. Some means +have to be employed to get rid of the greater part of +the heat and light. The simplest method of observing +is to fix a screen behind the eyepiece of a telescope +and let the image of the Sun be projected upon the +screen, or the sensitive plate may be substituted for +the screen, and a photograph obtained, which can be +examined at leisure afterwards. +</p> + +<p> +As generally seen, the surface of the Sun appears +to be mottled all over by a fine irregular stippling. +This stippling, though everywhere present, is not very +strongly marked, and a first hasty glance might +overlook it. From time to time, however, dark spots are +seen, of ever-changing form and size. By watching +these, Galileo proved that the Sun rotated on its axis +in a little more than twenty-five days, and in the +<span class="pagenum">{<a id="P69"></a>69}</span> +nineteenth century SCHWABE proved that the sunspots +were not equally large and numerous at all times, but +that there was a kind of cycle of a little more than +eleven years in average length. At one time the Sun +would be free from spots; then a few small ones would +appear; these would gradually become larger and more +numerous; then a decline would follow, and another +spotless period would succeed about eleven years after +the first. As a rule, the increase in the spots takes place +more quickly than the decline. +</p> + +<p> +Most of the spot-groups last only a very few days, +but about one group in four lasts long enough to be +brought round by the rotation of the Sun a second +time; in other words, it continues for about a month. +In a very few cases spots have endured for half a year. +</p> + +<p> +An ordinary form for a group of spots is a long +stream drawn out parallel to the Sun's equator, the +leading spot being the largest and best defined. It is +followed by a number of very small irregular and +ill-developed spots, and the train is brought up by a large +spot, sometimes even larger than the leader, but by no +means so regular in form or so well defined. The leading +spot for a short time moves forward much faster than +its followers, at a speed of about 8000 miles per day. +The small middle spots then gradually die out, or rather +seem to be overflowed by the bright material of the +solar surface, the "<b>photosphere</b>," as it is called; the spot +in the rear breaks up a little later, and the leader, which +is now almost circular, is left alone, and may last in this +condition for some weeks. Finally, it slowly contracts +or breaks up, and the disturbance comes to an end. +This is the course of development of many long-lived +spot-groups, but all do not conform to the same type. +<span class="pagenum">{<a id="P70"></a>70}</span> +The very largest spots are indeed usually quite different +in their appearance and history. +</p> + +<p> +In size, sunspots vary from the smallest dot that can +be discovered in the telescope up to huge rents with +areas that are to be counted by thousands of millions +of square miles; the great group of February 1905 +had an area of 4,000,000,000 square miles, a thousand +times the area of Europe. +</p> + +<p> +Closely associated with the <i>maculæ</i>, as the spots were +called by the first observers, are the "<b>faculæ</b>"—long, +branching lines of bright white light, bright as seen even +against the dazzling background of the Sun itself, and +looking like the long lines of foam of an incoming tide. +These are often associated with the spots; the spots +are formed between their ridges, and after a spot-group +has disappeared the broken waves of faculæ will +sometimes persist in the same region for quite a long +time. +</p> + +<p> +The faculæ clearly rise above the ordinary solar +surface; the spots as clearly are depressed a little below +it; because from time to time we see the bright material +of the surface pour over spots, across them, and +sometimes into them. But there is no reason to believe +that the spots are deep, in proportion either to the Sun +itself or even to their own extent. +</p> + +<p> +Sunspots are not seen in all regions of the Sun. It is +very seldom that they are noted in a higher solar +latitude than 40°, the great majority of spots lying in the +two zones between 5° and 25° latitude on either side +of the equator. Faculæ, on the other hand, though +most frequent in the spot zones, are observed much +nearer the two poles. +</p> + +<p> +It is very hard to find analogies on our Earth for +sunspots and for their peculiarities of behaviour. Some +<span class="pagenum">{<a id="P71"></a>71}</span> +of the earlier astronomers thought they were like +terrestrial volcanoes, or rather like the eruptions from +them. But if there were a solid nucleus to the Sun, +and the spots were eruptions from definite areas of the +nucleus, they would all give the same period of rotation. +But sunspots move about freely on the solar surface, +and the different zones of that surface rotate in different +times, the region of the equator rotating the most +quickly. This alone is enough to show that the Sun +is essentially not a solid body. Yet far down below +the photosphere something approaching to a definite +structure must already be forming. For there is a +well-marked progression in the zones of sunspots during +the eleven-year cycle. At a time when spots are few +and small, known as <b>the sunspot minimum</b>, they begin +to be seen in fairly high latitudes. As they get more +numerous, and many of them larger, they frequent the +medium zones. When the Sun is at its greatest activity, +known as <b>the sunspot maximum</b>, they are found from +the highest zone right down to the equator. Then the +decline sets in, but it sets in first in the highest zones, +and when the time of minimum has come again the +spots are close to the equator. Before these have all +died away, a few small spots, the heralds of a new +cycle of activity, begin to appear in high latitudes. +</p> + +<p> +This law, called after SPÖRER, its discoverer, indicates +that the origin and source of sunspot activity lie within +the Sun. At one time it was thought that sunspots +were due to some action of Jupiter—for Jupiter moves +round the Sun in 11.8 years, a period not very different +from the sunspot cycle—or to some meteoric stream. +But Spörer's Law could not be imposed by some +influence from without. Still sunspots, once formed, may +be influenced by the Earth, and perhaps by other +<span class="pagenum">{<a id="P72"></a>72}</span> +planets also, for MRS. WALTER MAUNDER has shown +that the numbers and areas of spots tend to be smaller +on the western half of the disc, as seen from the Earth, +than on the eastern, while considerably more groups +come into view at the east edge of the Sun than +pass out of view at the west edge, so that it would +appear as if the Earth had a damping effect upon the +spots exposed to it. +</p> + +<p> +But the Sun is far greater than it ordinarily appears +to us. Twice every year, and sometimes oftener, the +Moon, when new, comes between the Earth and the +Sun, and we have an <b>Eclipse of the Sun</b>, the dark body +of the Moon hiding part, or all, of the greater light. +The Sun and Moon are so nearly of the same apparent +size that an eclipse of the Sun is total only for a very +narrow belt of the Earth's surface, and, as the Moon +moves more quickly than the Sun, the eclipse only +remains total for a very short time—seven minutes at +the outside, more usually only two or three. North or +south of that belt the Moon is projected, so as to +leave uncovered a part of the Sun north or south of +the Moon. A total eclipse, therefore, is rare at any +particular place, and if a man were able to put himself +in the best possible position on each occasion, it would +cost him thirty years to secure an hour's accumulated +duration. +</p> + +<p> +Eclipses of the Moon are visible over half the world +at one time, for there is a real loss to the Moon of her +light. Her eclipses are brought about when, in her +orbit, she passes behind the Earth, and the Earth, being +between the Sun and the Moon, cuts off from the latter +most of the light falling upon her; not quite all; a +small portion reaches her after passing through the +thickest part of the Earth's atmosphere, so that the +<span class="pagenum">{<a id="P73"></a>73}</span> +Moon in an eclipse looks a deep copper colour, much as +she does when rising on a foggy evening. +</p> + +<p> +Total eclipses of the Sun have well repaid all the +efforts made to observe them. It is a wonderful sight +to watch the blackness of darkness slowly creeping over +the very fountain of light until it is wholly and entirely +hidden; to watch the colours fade away from the +landscape and a deathlike, leaden hue pervade all +nature, and then to see a silvery, star-like halo, flecked +with bright little rose-coloured flames, flash out round +the black disc that has taken the place of the Sun. +</p> + +<p> +These rose-coloured flames are the solar "<b>prominences</b>," +and the halo is the "<b>corona</b>," and it is to watch these +that astronomers have made so many expeditions hither +and thither during the last seventy years. The +"prominences," or red flames, can be observed, without an +eclipse, by means of the spectroscope, but, as the work +of the spectroscope is to form the subject of another +volume of this series, it is sufficient to add here that +the prominences are composed of various glowing gases, +chiefly of hydrogen, calcium, and helium. +</p> + +<p> +These and other gases form a shell round the Sun, +about 3000 miles in depth, to which the name "<b>chromosphere</b>" +has been given. It is out of the chromosphere +that the prominences arise as vast irregular jets and +clouds. Ordinarily they do not exceed 40 or 50 thousand +miles in height, but occasionally they extend for 200 +or even 300 thousand miles from the Sun. Their +changes are as remarkable as their dimensions; huge +jets of 50 or 100 thousand miles have been seen to +form, rise, and disappear within an hour or less, and +movements have been chronicled of 200 or 300 miles +in a single second of time. +</p> + +<p> +Prominences are largest and most frequent when +<span class="pagenum">{<a id="P74"></a>74}</span> +sunspots and faculæ are most frequent, and fewest +when those are fewest. The corona, too, varies with +the sunspots. At the time of maximum the corona +sends forth rays and streamers in all directions, and +looks like the conventional figure of a star on a gigantic +scale. At minimum the corona is simpler in form, and +shows two great wings, east and west, in the direction +of the Sun's equator, and round both of his poles a +number of small, beautiful jets like a crest of feathers. +</p> + +<p> +Some of the streamers or wings of the corona have +been traced to an enormous distance from the Sun. +Mrs. Walter Maunder photographed one ray of the +corona of 1898 to a distance of 6 millions of miles. +LANGLEY, in the clear air of Pike's Peak, traced the +wings of the corona of 1878 with the naked eye to +nearly double this distance. +</p> + +<p> +But the rapid changes of sunspots and the violence +of some of the prominence eruptions are but feeble +indications of the most wonderful fact concerning the +Sun, <i>i.e.</i> the enormous amount of light and heat which +it is continually giving off. Here we can only put +together figures which by their vastness escape our +understanding. Sunlight is to moonlight as 600,000 is +to 1, so that if the entire sky were filled up with full +moons, they would not give us a quarter as much light +as we derive from the Sun. The intensity of sunlight +exceeds by far any artificial light; it is 150 times as +bright as the calcium light, and three or four times as +bright as the brightest part of the electric arc light. +The amount of heat radiated by the Sun has been +expressed in a variety of different ways; C. A. YOUNG very +graphically by saying that if the Sun were encased in +a shell of ice 64 feet deep, its heat would melt the shell +in one minute, and that if a bridge of ice could be +<span class="pagenum">{<a id="P75"></a>75}</span> +formed from the Earth to the Sun, 2-½ miles square in +section and 93 millions of miles long, and the entire +solar radiation concentrated upon it, in one second the +ice would be melted, in seven more dissipated into +vapour. +</p> + +<p> +The Earth derives from the Sun not merely light +and heat, but, by transformation of these, almost every +form of energy manifest upon it; the energy of the +growth of plants, the vital energy of animals, are only +the energy received from the Sun, changed in its +expression. +</p> + +<p> +The question naturally arises, "If the Sun, to which +the Earth is indebted for nearly everything, passes +through a change in its activity every eleven years or +so, how is the Earth affected by it?" It would seem +at first sight that the effect should be great and +manifest. A sunspot, like that of February 1905, one +thousand times as large as Europe, into which worlds +as large as our Earth might be poured, like peas into a +saucer, must mean, one might think, an immense +falling off of the solar heat. +</p> + +<p> +Yet it is not so. For even this great sunspot was +but small as compared with the Sun as a whole. Had +it been dead black, it would have stopped out much +less than 1 per cent. of the Sun's heat; and even the +darkest sunspot is really very bright. And the more +spots there are, the more numerous and brighter are +the faculæ; so that we do not know certainly which of +the two phases, maximum or minimum, means the +greater radiation. If the weather on the Earth answers +to the sunspot cycle, the connection is not a simple +one; as yet no connection has been proved. Thus +two of the worst and coldest summers experienced in +England fell the one in 1860, the other in 1879, <i>i.e.</i> at +<span class="pagenum">{<a id="P76"></a>76}</span> +maximum and minimum respectively. So, too, the hot +summers of 1893 and 1911 were also, the one at +maximum and the other at minimum; and ordinary +average years have fallen at both the phases just the +same. +</p> + +<p> +Yet there is an answer on the part of the Earth to +these solar changes. The Earth itself is a kind of +magnet, possessing a magnetism of which the intensity +and direction is always changing. To watch these +changes, very sensitive magnets are set up, and a slight +daily to-and-fro swing is noticed in them; this swing is +more marked in summer than in winter, but it is also +more marked at times of the sunspot maximum than +at minimum, showing a dependence upon the solar +activity. +</p> + +<p> +Yet more, from time to time the magnetic needle +undergoes more or less violent disturbance; in extreme +cases the electric telegraph communication has been +disturbed all over the world, as on September 25, 1909, +when the submarine cables ceased to carry messages +for several hours. In most cases when such a "magnetic +storm" occurs, there is an unusually large or active +spot on the Sun. The writer was able in 1904 to +further prove that such "storms" have a marked +tendency to recur when the same longitude of the Sun +is presented again towards the Earth. Thus in +February 1892, when a very large spot was on the +Sun, a violent magnetic storm broke out. The spot +passed out of sight and the storm ceased, but in the +following month, when the spot reached exactly the +same apparent place on the Sun's disc, the storm broke +out again. Such magnetic disturbances are therefore +due to streams of particles driven off from limited areas +of the Sun, probably in the same way that the long, +<span class="pagenum">{<a id="P77"></a>77}</span> +straight rays of the corona are driven off. Such streams +of particles, shot out into space, do not spread out +equally in all directions, like the rays of light and heat, +but are limited in direction, and from time to time +they overtake the Earth in its orbit, and, striking it, +cause a magnetic storm, which is felt all over the Earth +at practically the same moment. +</p> + +<p> +JUPITER is, after the Sun, much the largest member +of the solar system, and it is a peculiarly beautiful +object in the telescope. Even a small instrument shows +the little disc striped with many delicately coloured +bands or belts, broken by white clouds and dark streaks, +like a "windy sky" at sunset. And it changes while +being watched, for, though 400,000,000 miles away from +us, it rotates so fast upon its axis that its central +markings can actually be seen to move. +</p> + +<p> +This rapid rotation, in less than ten hours, is the +most significant fact about Jupiter. For different spots +have different rotation periods, even in the same +latitude, proving that we are looking down not upon any +solid surface of Jupiter, but upon its cloud envelope—an +envelope swept by its rapid rotation and by its winds +into a vast system of parallel currents. +</p> + +<p> +One object on Jupiter, the great "<b>Red Spot</b>," has been +under observation since 1878, and possibly for 200 years +before that. It is a large, oval object fitted in a frame +of the same shape. The spot itself has often faded and +been lost since 1878, but the frame has remained. The +spot is in size and position relative to Jupiter much as +Australia is to the Earth, but while Australia moves +solidly with the rest of the Earth in the daily +rotation, neither gaining on South America nor losing +on Africa, the Red Spot on Jupiter sees many +other spots and clouds pass it by, and does not even +<span class="pagenum">{<a id="P78"></a>78}</span> +retain the same rate of motion itself from one year to +another. +</p> + +<p> +No other marking on Jupiter is so permanent as this. +From time to time great round white clouds form in a +long series as if shot up from some eruption below, and +then drawn into the equatorial current. From time to +time the belts themselves change in breadth, in colour, +and complexity. Jupiter is emphatically the planet of +change. +</p> + +<p> +And such change means energy, especially energy in +the form of heat. If Jupiter possessed no heat but +that it derived from the Sun, it would be colder than +Mars, and therefore an absolutely frozen globe. But +these rushing winds and hurrying clouds are evidences +of heat and activity—a native heat much above that +of our Earth. While Mars is probably nearer to the +Moon than to the Earth in its condition, Jupiter has +probably more analogies with the Sun. +</p> + +<p> +The one unrivalled distinction of SATURN is its Ring. +Nothing like this exists elsewhere in the solar system. +Everywhere else we see spherical globes; this is a flat +disc, but without its central portion. It surrounds the +planet, lying in the plane of its equator, but touches it +nowhere, a gap of 7000 miles intervening. It appears +to be circular, and is 42,000 miles in breadth. +</p> + +<p> +Yet it is not, as it appears to be, a flat continuous +surface. It is in reality made up of an infinite number +of tiny satellites, mere dust or pebbles for the most +part, but so numerous as to look from our distance like +a continuous ring, or rather like three or four concentric +rings, for certain divisions have been noticed in it—an +inner broad division called after its discoverer, CASSINI, +and an outer, fainter, narrower one discovered by +ENCKE. The innermost part of the ring is dusky, fainter +<span class="pagenum">{<a id="P79"></a>79}</span> +than the planet or the rest of the ring, and is known as +the "crape-ring." +</p> + +<p> +Of Saturn itself we know little; it is further off and +fainter than Jupiter, and its details are not so +pronounced, but in general they resemble those of Jupiter. +The planet rotates quickly—in 10 h. 14 m.—its markings +run into parallel belts, and are diversified by spots +of the same character as on Jupiter. Saturn is +probably possessed of no small amount of native heat. +</p> + +<p> +URANUS and NEPTUNE are much smaller bodies than +Jupiter and Saturn, though far larger than the Earth. +But their distance from the Earth and Sun makes their +discs small and faint, and they show little in the +telescope beyond a hint of "belts" like those of Jupiter; +so that, as with that planet, the surfaces that they +show are almost certainly the upper surfaces of a shell +of cloud. +</p> + +<p> +In general, therefore, the rule appears to hold good +throughout the solar system that a very large body is +intensely hot and in a condition of violent activity and +rapid change; that smaller bodies are less hot and less +active, until we come down to the smallest, which are +cold, inert, and dead. Our own Earth, midway in the +series, is itself cold, but is placed at such a distance +from the Sun as to receive from it a sufficient but not +excessive supply of light and heat, and the changes of +the Earth are such as not to prohibit but to nourish +and support the growth and development of the various +forms of life. +</p> + +<p> +The smallest members of the solar system are known +as METEORS. These are often no more than pebbles +or particles of dust, moving together in associated orbits +round the Sun. They are too small and too scattered +to be seen in open space, and become visible to us only +<span class="pagenum">{<a id="P80"></a>80}</span> +when their orbits intersect that of the earth, and the +earth actually encounters them. They then rush into +our atmosphere at a great speed, and become highly +heated and luminous as they compress the air before +them; so highly heated that most are vapourised and +dissipated, but a few reach the ground. As they are +actually moving in parallel paths at the time of one of +these encounters, they appear from the effect of +perspective to diverge from a point, hence called the +"<b>radiant</b>." Some showers occur on the same date of +every year; thus a radiant in the constellation Lyra is +active about April 21, giving us meteors, known as +the "Lyrids"; and another in Perseus in August, +gives us the "Perseids." Other radiants are active +at intervals of several years; the most famous of all +meteoric showers, that of the "Leonids," from a radiant +in Leo, was active for many centuries every thirty-third +year; and another falling in the same month, November, +came from a radiant in Andromeda every thirteen years. +In these four cases and in some others the meteors +have been found to be travelling along the same path +as a comet. It is therefore considered that meteoric +swarms are due to the gradual break up of comets; +indeed the comet of the Andromeda shower, known +from one of its observers as "Biela's," was actually +seen to divide into two in December 1845, and has not +been observed as a comet since 1852, though the showers +connected with it, giving us the meteors known as the +"Andromedes," have continued to be frequent and rich. +Meteors, therefore, are the smallest, most insignificant, +of all the celestial bodies; and the shining out of a +meteor is the last stage of its history—its death; after +death it simply goes to add an infinitesimal trifle to the +dust of the earth. +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap06"></a></p> + +<p><span class="pagenum">{<a id="P81"></a>81}</span></p> + +<h3> +CHAPTER VI +</h3> + +<h3> +THE SYSTEM OF THE STARS +</h3> + +<p> +The first step towards our knowledge of the starry +heavens was made when the unknown and forgotten +astronomers of 2700 B.C. arranged the stars into +constellations, for it was the first step towards +distinguishing one star from another. When one star began +to be known as "the star in the eye of the Bull," and +another as "the star in the shoulder of the Giant," +the heavens ceased to display an indiscriminate crowd +of twinkling lights; each star began to possess +individuality. +</p> + +<p> +The next step was taken when Hipparchus made +his catalogue of stars (129 B.C.), not only giving its +name to each star, but measuring and fixing its +place—a catalogue represented to us by that of Claudius +Ptolemy (A.D. 137). +</p> + +<p> +The third step was taken when BRADLEY, the third +Astronomer Royal, made, at Greenwich, a catalogue of +more than 3000 star-places determined with the telescope. +</p> + +<p> +A century later ARGELANDER made the great Bonn +Zone catalogue of 330,000 stars, and now a great +photographic catalogue and chart of the entire heavens +have been arranged between eighteen observatories of +different countries. This great chart when complete +will probably present 30 millions of stars in position +and brightness. +</p> + +<p> +<span class="pagenum">{<a id="P82"></a>82}</span> +</p> + +<p> +The question naturally arises, "Why so many stars? +What conceivable use can be served by catalogues of +30 millions or even of 3000 stars?" And so far as +strictly practical purposes are concerned, the answer +must be that there is none. Thus MASKELYNE, the +fifth Astronomer Royal, restricted his observations to +some thirty-six stars, which were all that he needed +for his <i>Nautical Almanac</i>, and these, with perhaps a +few additions, would be sufficient for all purely practical +ends. +</p> + +<p> +But there is in man a restless, resistless passion for +knowledge—for knowledge for its own sake—that is +always compelling him to answer the challenge of the +unknown. The secret hid behind the hills, or across the +seas, has drawn the explorer in all ages; and the secret +hid behind the stars has been a magnet not less powerful. +So catalogues of stars have been made, and made again, +and enlarged and repeated; instruments of ever-increasing +delicacy have been built in order to determine the +positions of stars, and observations have been made +with ever-increasing care and refinement. It is +knowledge for its own sake that is longed for, knowledge +that can only be won by infinite patience and care. +</p> + +<p> +The chief instrument used in making a star catalogue +is called a transit circle; two great stone pillars are set +up, each carrying one end of an axis, and the axis carries +a telescope. The telescope can turn round like a wheel, +in one direction only; it points due north or due south. +A circle carefully divided into degrees and fractions of +a degree is attached to the telescope. +</p> + +<p> +In the course of the twenty-four hours every star +above the horizon of the observatory must come at +least once within the range of this telescope, and at +that moment the observer points the telescope to the +<span class="pagenum">{<a id="P83"></a>83}</span> +star, and notes the time by his clock when the star +crossed the spider's threads, which are fitted in the +focus of his eye-piece. He also notes the angle at +which the telescope was inclined to the horizon by +reading the divisions of his circle. For by these +two—the time when the star passed before the telescope +and the angle at which the telescope was inclined—he +is able to fix the position of the star. +</p> + +<p> +"But why should catalogues be repeated? When +once the position of a star has been observed, why +trouble to observe it again? Will not the record serve +in perpetuity?" +</p> + +<p> +The answers to these questions have been given by +star catalogues themselves, or have come out in the +process of making them. The Earth rotates on its axis +and revolves round the Sun. But that axis also has a +rolling motion of its own, and gives rise to an apparent +motion of the stars called <b>Precession</b>. Hipparchus +discovered this effect while at work on his catalogue, and +our knowledge of the amount of Precession enables us +to fix the date when the constellations were designed. +</p> + +<p> +Similarly, Bradley discovered two further apparent +motions of the stars—<b>Aberration</b> and <b>Nutation</b>. Of +these, the first arises from the fact that the light coming +from the stars moves with an inconceivable speed, but +does not cross from star to Earth instantly; it takes +an appreciable, even a long, time to make the journey. +But the Earth is travelling round the Sun, and +therefore continually changing its direction of motion, and +in consequence there is an apparent change in the +direction in which the star is seen. The change is very +small, for though the Earth moves 18-½ miles in a second, +light travels 10,000 times as fast. Stars therefore are +deflected from their true positions by Aberration, by +<span class="pagenum">{<a id="P84"></a>84}</span> +an extreme amount of 20.47" of arc, that being the +angle shown by an object that is slightly more distant +than 10,000 times its diameter. +</p> + +<p> +The axis of the Earth not only rolls on itself, but it +does so with a slight staggering, nodding motion, due +to the attractions of the Sun and Moon, known as +<b>Nutation</b>. And the axis does not remain fixed in the +solid substance of the Earth, but moves about +irregularly in an area of about 60 feet in diameter. The +positions of the north and south poles are therefore not +precisely fixed, but move, producing what is known as +the <b>Variation of Latitude</b>. Then star-places have to +be corrected for the effect of our own atmosphere, +<i>i.e.</i> refraction, and for errors of the instruments by which +their places are determined. And when all these have +been allowed for, the result stands out that different +stars have real movement of their own—their <b>Proper +Motions</b>. +</p> + +<p> +No stars are really "fixed"; the name "<b>fixed stars</b>" +is a tradition of a time when observation was too rough +to detect that any of the heavenly bodies other than +the planets were in motion. But nothing is fixed. +The Earth on which we stand has many different +motions; the stars are all in headlong flight. +</p> + +<p> +And from this motion of the stars it has been learned +that the Sun too moves. When Copernicus overthrew +the Ptolemaic theory and showed that the Earth moves +round the Sun, it was natural that men should be +satisfied to take this as the centre of all things, fixed +and immutable. It is not so. Just as a traveller +driving through a wood sees the trees in front +apparently open out and drift rapidly past him on either +hand, and then slowly close together behind him, so +Sir WILLIAM HERSCHEL showed that the stars in one +<span class="pagenum">{<a id="P85"></a>85}</span> +part of the heavens appear to be opening out, or slowly +moving apart, while in the opposite part there seems +to be a slight tendency for them to come together, +and in a belt midway between the two the tendency +is for a somewhat quicker motion toward the second +point. And the explanation is the same in the one +case as in the other—the real movement is with the +observer. The Sun with all its planets and smaller +attendants is rushing onward, onward, towards a point +near the borders of the constellations Lyra and +Hercules, at the rate of about twelve miles per second. +</p> + +<p> +Part of the Proper Motions of the stars are thus only +apparent, being due to the actual motion of the Sun—the +"<b>Sun's Way</b>," as it is called—but part of the Proper +Motions belong to the stars themselves; they are really +in motion, and this not in a haphazard, random manner. +For recently KAPTEYN and other workers in the same +field have brought to light the fact of <b>Star-Drift</b>, <i>i.e.</i> that +many of the stars are travelling in associated +companies. This may be illustrated by the seven bright +stars that make up the well-known group of the +"Plough," or "Charles's Wain," as country people call +it. For the two stars of the seven that are furthest +apart in the sky are moving together in one direction, +and the other five in another. +</p> + +<p> +Another result of the close study of the heavens +involved in the making of star catalogues has been the +detection of DOUBLE STARS—stars that not only appear +to be near together but are really so. Quite a distinct +and important department of astronomy has arisen +dealing with the continual observation and measurement +of these objects. For many double stars are in +motion round each other in obedience to the law of +gravitation, and their orbits have been computed. +<span class="pagenum">{<a id="P86"></a>86}</span> +Some of these systems contain three or even four +members. But in every case the smaller body shines +by its own light; we have no instance in these double +stars of a sun attended by a planet; in each case it +is a sun with a companion sun. The first double star +to be observed as such was one of the seven stars of the +Plough. It is the middle star in the Plough handle, +and has a faint star near it that is visible to any +ordinarily good sight. +</p> + +<p> +Star catalogues and the work of preparing them have +brought out another class—VARIABLE STARS. As the +places of stars are not fixed, so neither are their +brightnesses, and some change their brightness quickly, even +as seen by the naked eye. One of these is called <b>Algol</b>, +<i>i.e.</i> the Demon Star, and is in the constellation Perseus. +The ancient Greeks divided all stars visible to the +naked eye into six classes, or "<b>magnitudes</b>," according to +their brightness, the brightest stars being said to be +of the first magnitude, those not quite so bright of the +second, and so on. Algol is then usually classed as a +star of the second magnitude, and for two days and a +half it retains its brightness unchanged. Then it begins +to fade, and for four and a half hours its brightness +declines, until two-thirds of it has gone. No further +change takes place for about twenty minutes, after which +the light begins to increase again, and in another four +and a half hours it is as bright as ever, to go through +the same changes again after another interval of two +days and a half. +</p> + +<p> +Algol is a double star, but, unlike those stars that we +know under that name, the companion is dark, but is +nearly as large as its sun, and is very close to it, moving +round it in a little less than three days. At one point +of its orbit it comes between Algol and the Earth, +<span class="pagenum">{<a id="P87"></a>87}</span> +and Algol suffers, from our point of view, a partial +eclipse. +</p> + +<p> +There are many other cases of variable stars of this +kind in which the variation is caused by a dark +companion moving round the bright star, and eclipsing it +once in each revolution; and the diameters and +distances of some of these have been computed, showing +that in some cases the two stars are almost in contact. +In some instances the companion is a dull but not a +dark star; it gives a certain amount of light. When +this is the case there is a fall of light twice in the +period—once when the fainter star partly eclipses the brighter, +once when the brighter star partly eclipses the fainter. +</p> + +<p> +But not all variable stars are of this kind. There is +a star in the constellation Cetus which is sometimes of +the second magnitude, at which brightness it may remain +for about a fortnight. Then it will gradually diminish +in brightness for nine or ten weeks, until it is lost to the +unassisted sight, and after six months of invisibility it +reappears and increases during another nine or ten +weeks to another maximum. "Mira," <i>i.e.</i> wonderful +star, as this variable is called, is about 1000 times as +bright at maximum as at minimum, but some maxima +are fainter than others; neither is the period of +variation always the same. It is clear that variation of this +kind cannot be caused by an eclipse, and though many +theories have been suggested, the "<b>long-period variables</b>," +of which Mira is the type, as yet remain without a +complete explanation. +</p> + +<p> +More remarkable still are the "NEW STARS"—stars +that suddenly burst out into view, and then quickly +fade away, as if a beacon out in the stellar depths +had suddenly been fired. One of these suggested +to Hipparchus the need for a catalogue of the +<span class="pagenum">{<a id="P88"></a>88}</span> +stars; another, the so-called "Pilgrim Star," in the +year 1572 was the means of fixing the attention of +Tycho Brahe upon astronomy; a third in 1604 was +observed and fully described by Kepler. The real +meaning of these "new," or "temporary," stars was +not understood until the spectroscope was applied to +astronomy. They will therefore be treated in the +volume of this series to be devoted to that subject. +It need only be mentioned here that their appearance +is evidently due to some kind of collision between +celestial bodies, producing an enormous and +instantaneous development of light and heat. +</p> + +<p> +These New Stars do not occur in all parts of the +heavens. Even a hasty glance at the sky will show +that the stars are not equally scattered, but that a +broad belt apparently made up of an immense number +of very small stars divides them into two parts. +</p> + +<p> +THE MILKY WAY, or GALAXY, as this belt is called, +bridges the heavens at midnight, early in October, like +an enormous arch, resting one foot on the horizon in +the east, and the other in the west, and passing through +the "<b>Zenith</b>," <i>i.e.</i> the point overhead. It is on this belt +of small stars—on the Milky Way—that New Stars are +most apt to break out. +</p> + +<p> +The region of the Milky Way is richer in stars than +are the heavens in general. But it varies itself also +in richness in a remarkable degree. In some places the +stars, as seen on some of the wonderful photographs +taken by E. E. BARNARD, seem almost to form a +continuous wall; in other places, close at hand, barren +spots appear that look inky black by contrast. And +the <b>Star Clusters</b>, stars evidently crowded together, are +frequent in the Milky Way. +</p> + +<p> +And yet again beside the stars the telescope reveals +<span class="pagenum">{<a id="P89"></a>89}</span> +to us the NEBULÆ. Some of these are the Irregular +Nebulæ—wide-stretching, cloudy, diffused masses of +filmy light, like the Great Nebula in Orion. Others +are faint but more defined objects, some of them with +small circular discs, and looking like a very dim +Uranus, or even like Saturn—that is to say, like a +planet with a ring round its equator. This class are +therefore known as "<b>Planetary Nebulæ</b>," and, when bright +enough to show traces of colour, appear green or greenish +blue. +</p> + +<p> +These are, however, comparatively rare. Other of +these faint, filmy objects are known as the "<b>White +Nebulæ</b>," and are now counted by thousands. They +affect the spiral form. Sometimes the spiral is seen +fully presented; sometimes it is seen edgewise; +sometimes more or less foreshortened, but in general the +spiral character can be detected. And these White +Nebulæ appear to shun the Galaxy as much as the +Planetary Nebula; and Star Clusters prefer it; indeed +the part of the northern heavens most remote from the +Milky Way is simply crowded with them. +</p> + +<p> +It can be by no accident or chance that in the vast +edifice of the heavens objects of certain classes should +crowd into the belt of the Milky Way, and other classes +avoid it; it points to the whole forming a single +growth, an essential unity. For there is but one belt +in the heavens, like the Milky Way, a belt in which +small stars, New Stars, and Planetary Nebulæ find their +favourite home; and that belt encircles the entire +heavens; and similarly that belt is the only region +from which the White Nebulæ appear to be repelled. +The Milky Way forms the foundation, the strong and +buttressed wall of the celestial building; the White +Nebulæ close in the roof of its dome. +</p> + +<p> +<span class="pagenum">{<a id="P90"></a>90}</span> +</p> + +<p> +And how vast may that structure be—how far is it +from wall to wall? +</p> + +<p> +That, as yet, we can only guess. But the stars whose +distances we can measure, the stars whose drifting we +can watch, almost infinitely distant as they are, carry +us but a small part of the way. Still, from little hints +gathered here and there, we are able to guess that, +though the nearest star to us is nearly 300,000 times +as far as the Sun, yet we must overpass the distance of +that star 1000 times before we shall have reached the +further confines of the Galaxy. Nor is the end in sight +even there. +</p> + +<p> +This is, in briefest outline, the Story of Astronomy. +It has led us from a time when men were acquainted +with only a few square miles of the Earth, and knew +nothing of its size and shape, or of its relation to the +moving lights which shone down from above, on to +our present conception of our place in a universe of +suns of which the vastness, glory, and complexity +surpass our utmost powers of expression. The science +began in the desire to use Sun, Moon, and stars as +timekeepers, but as the exercise of ordered sight and +ordered thought brought knowledge, knowledge began +to be desired, not for any advantage it might bring, +but for its own sake. And the pursuit itself has brought +its own reward in that it has increased men's powers, +and made them keener in observation, clearer in +reasoning, surer in inference. The pursuit indeed knows no +ending; the questions to be answered that lie before +us are now more numerous than ever they have been, +and the call of the heavens grows more insistent: +</p> + +<p class="t3"> + "LIFT UP YOUR EYES ON HIGH."<br /> +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap07"></a></p> + +<p><span class="pagenum">{<a id="P91"></a>91}</span></p> + +<h3> +BOOKS TO READ +</h3> + +<p><br /></p> + +<p class="noindent"> +POPULAR GENERAL DESCRIPTIONS:— +</p> + +<p class="noindent"> + Sir R. S. Ball.—<i>Star-Land</i>. (Cassell.)<br /> + Agnes Giberne.—-Sun, Moon and Stars<i>. (Seeley.)<br /> + W. T. Lynn.—</i>Celestial Motions<i>. (Stanford.)<br /> + A. & W. Maunder.—-The Heavens and their Story</i>. (Culley.)<br /> + Simon Newcomb.—<i>Astronomy for Everybody</i>. (Isbister.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +FOR BEGINNERS IN OBSERVATION:— +</p> + +<p class="noindent"> + W. F. Denning.—<i>Telescopic Work for Starlight Evenings</i>. (Taylor & Francis.)<br /> + E. W. Maunder.—<i>Astronomy without a Telescope</i>. (Thacker.)<br /> + Arthur P. Norton.—<i>A Star Atlas and Telescopic Handbook</i>. (Gall & Inglis.) <br /> + Garrett P. Serviss.—<i>Astronomy with an Opera-Glass</i>. (Appleton.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +STAR-ATLASES:— +</p> + +<p class="noindent"> + Rev. J. Gall—<i>An Easy Guide to the Constellations</i>. (Gall and Inglis.)<br /> + E. M'Clure and H. J. Klein.—<i>Star-Atlas</i>. (Society for Promoting Christian Knowledge.)<br /> + R. A. Proctor.—<i>New Star Atlas</i>. (Longmans.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +ASTRONOMICAL INSTRUMENTS AND METHODS:— +</p> + +<p class="noindent"> + Sir G. B. Airy.—<i>Popular Astronomy; Lectures delivered at Ipswich</i>. (Macmillan.)<br /> + E. W. Maunder.—<i>Royal Observatory, Greenwich; its History and Work</i>. (Religious Tract Society.)<br /> +</p> + +<p><br /></p> + +<p> +<span class="pagenum">{<a id="P92"></a>92}</span> +</p> + +<p><br /></p> + +<p class="noindent"> +GENERAL TEXT-BOOKS:— +</p> + +<p class="noindent"> + Clerke, Fowler & Gore.—Concise Astronomy. (Hutchinson.)<br /> + Simon Newcomb.—Popular Astronomy. (Macmillan.)<br /> + C. A. Young.—Manual of Astronomy. (Ginn.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +SPECIAL SUBJECTS:— +</p> + +<p class="noindent"> + Rev. E. Ledger.—<i>The Sun; its Planets and Satellites</i>. (Stanford.)<br /> + C. A. Young.—<i>The Sun</i>. (Kegan Paul.)<br /> + Mrs. Todd.—<i>Total Eclipses</i>. (Sampson Low.)<br /> + Nasmyth and Carpenter.—<i>The Moon</i>. (John Murray.)<br /> + Percival Lowell.—<i>Mars</i>. (Longmans.)<br /> + Ellen M. Clerke.—<i>Jupiter</i>. (Stanford.)<br /> + E. A. Proctor.—<i>Saturn and its System</i>. (Longmans.)<br /> + W. T. Lynn.—<i>Remarkable Comets</i>. (Stanford.)<br /> + E. W. Maunder.—<i>The Astronomy of the Bible</i>. (Hodder and Stoughton.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +HISTORICAL:— +</p> + +<p class="noindent"> + W. W. Bryant.—<i>History of Astronomy</i>. (Methuen.)<br /> + Agnes M. Clerke.—<i>History of Astronomy in the Nineteenth Century</i>. (A. & C. Black.)<br /> + George Forbes.—<i>History of Astronomy</i>. (Watts.)<br /> +</p> + +<p><br /></p> + +<p class="noindent"> +BIOGRAPHICAL:— +</p> + +<p class="noindent"> + Sir E. S. Ball.—<i>Great Astronomers</i>. (Isbister.)<br /> + Agnes M. Clerke.—<i>The Herschels and Modern Astronomy</i>. (Cassell.)<br /> + Sir O. Lodge.—<i>Pioneers of Science</i>. (Macmillan.)<br /> +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap08"></a></p> + +<p><span class="pagenum">{<a id="P93"></a>93}</span></p> + +<h3> +INDEX +</h3> + +<pre class="index"> + ABERRATION, <a href="#P83">83</a> + "Achilles" (Minor planet), <a href="#P38">38</a> + Adams, John C., <a href="#P39">39</a> + Airy, <a href="#P39">39</a> + "Algol," <a href="#P86">86</a> + "Andromedes" (Meteors), <a href="#P80">80</a> + Apsides, <a href="#P24">24</a>, <a href="#P28">28</a> + Argelander, <a href="#P81">81</a> + + + BARNARD, E. E., <a href="#P88">88</a> + "Bear," The, <a href="#P14">14</a> + Biela's Comet, <a href="#P80">80</a> + Bouvard, <a href="#P39">39</a> + Bradley, <a href="#P81">81</a>, <a href="#P83">83</a> + Bremiker, <a href="#P40">40</a> + + + CATALOGUES (star), <a href="#P81">81-83</a> + Centauri, Alpha, <a href="#P53">53</a> + "Ceres" (Minor planet), <a href="#P38">38</a> + Challis, <a href="#P40">40</a> + Charles II., <a href="#P50">50</a> + Chromosphere, <a href="#P73">73</a> + Chronometer, <a href="#P50">50</a> + Clairaut, <a href="#P36">36</a> + Columbus, <a href="#P48">48</a> + Comets, <a href="#P36">36</a> + Comet, Halley's, <a href="#P37">37</a> + ---- Biela's, <a href="#P80">80</a> + Conic Sections, <a href="#P34">34</a> + Constellations, the, <a href="#P15">15</a> + ---- date of, <a href="#P16">16</a> + Cook, Capt., <a href="#P50">50</a> + Copernicus, <a href="#P26">26</a>, <a href="#P54">54</a>, <a href="#P84">84</a> + "Copernicus" (Lunar crater), <a href="#P59">59</a>, <a href="#P60">60</a> + Corona, <a href="#P73">73</a> + Cowell, <a href="#P37">37</a> + Crommelin, <a href="#P37">37</a> + + + DEGREES, <a href="#P43">43</a> + Dollond, <a href="#P47">47</a> + Double stars, <a href="#P85">85</a> + + + EARTH, form of, <a href="#P16">16</a> + ---- size of, <a href="#P17">17</a>, <a href="#P33">33</a> + Eclipses, <a href="#P72">72</a> + Ecliptic, <a href="#P21">21</a> + Ellipse, <a href="#P28">28</a> + Epicycle, <a href="#P25">25</a> + Eratosthenes, <a href="#P17">17</a> + "Eros" (Minor planet), <a href="#P38">38</a>, <a href="#P52">52</a> + Eudoxus, <a href="#P21">21</a> + Excentric, <a href="#P24">24</a> + Eye-piece, <a href="#P45">45</a> + + + FACULÆ, <a href="#P70">70</a> + Flamsteed, <a href="#P50">50</a> + + + GALILEO, <a href="#P44">44</a> + Galle, <a href="#P40">40</a> + Gascoigne, <a href="#P46">46</a> + Gravitation, Law of, <a href="#P34">34</a> + + + HALL, CHESTER MOOR, <a href="#P47">47</a> + Halley, <a href="#P36">36</a> + Halley's Comet, <a href="#P37">37</a> + Harrison, John, <a href="#P50">50</a> + Herschel, Sir W., <a href="#P37">37</a>, <a href="#P47">47</a>, <a href="#P84">84</a> + Hipparchus, <a href="#P24">24</a>, <a href="#P81">81</a>, <a href="#P83">83</a>, <a href="#P87">87</a> + Hyperbola, <a href="#P34">34</a> + + + JOB, Book of, <a href="#P12">12</a>, <a href="#P14">14</a> + "Juno" (Minor planet), <a href="#P38">38</a> + Jupiter, <a href="#P18">18</a>, <a href="#P32">32</a>, <a href="#P77">77-78</a> + + + KAPTEYN, <a href="#P85">85</a> + Kepler, <a href="#P28">28</a>, <a href="#P44">44</a>, <a href="#P88">88</a> + Kepler's Laws, <a href="#P29">29</a> + "Kepler" (Lunar crater), <a href="#P59">59</a> + + + LANGLEY, <a href="#P74">74</a> + Latitude, Variation of, <a href="#P84">84</a> + "Leonids" (Meteors), <a href="#P80">80</a> + Leverrier, <a href="#P39">39</a> + Lowell, <a href="#P63">63</a>, <a href="#P64">64</a> + "Lyrids" (Meteors), <a href="#P80">80</a> + + + MAGNETIC STORM, <a href="#P76">76</a> + Magnetism, Earth's, <a href="#P76">76</a> + Magnitudes of stars, <a href="#P86">86</a> + "Mare Imbrium," <a href="#P59">59</a> + Mars, <a href="#P18">18</a>, <a href="#P52">52</a>, <a href="#P62">62-66</a> + ---- Canals of, <a href="#P63">63</a> + Maskelyne, <a href="#P50">50</a>, <a href="#P82">82</a> + Maunder, Mrs. Walter, <a href="#P72">72</a>, <a href="#P74">74</a> + Mercury, <a href="#P17">17</a>, <a href="#P18">18</a>, <a href="#P27">27</a>, <a href="#P32">32</a>, <a href="#P66">66-67</a> + Meteors, <a href="#P79">79</a>, <a href="#P80">80</a> + Micrometer, <a href="#P46">46</a> + Milky Way, <a href="#P53">53</a>, <a href="#P88">88</a> + Minor Planets, <a href="#P38">38</a>, <a href="#P52">52</a> + Minutes of arc, <a href="#P44">44</a> + "Mira," <a href="#P87">87</a> + Moon, <a href="#P11">11</a>, <a href="#P14">14</a>, <a href="#P21">21</a>, <a href="#P32">32</a>, <a href="#P33">33</a>, <a href="#P49">49</a>, <a href="#P55">55-62</a> + ---- distance of, <a href="#P51">51</a> + + + "<i>Nautical Almanac</i>," <a href="#P50">50</a>, <a href="#P82">82</a> + Navigation, <a href="#P49">49</a> + Nebulæ, <a href="#P89">89</a> + Neptune, <a href="#P40">40</a>, <a href="#P79">79</a> + Newcomb, <a href="#P65">65</a> + New stars, <a href="#P87">87</a> + Newton, <a href="#P29">29</a>, <a href="#P31">31</a>, <a href="#P47">47</a> + Newton's Laws of motion, <a href="#P31">31</a> + Nodes, <a href="#P35">35</a> + Nutation, <a href="#P83">83</a>, <a href="#P84">84</a> + + + "OASES of Mars," <a href="#P64">64</a> + Obelisks, <a href="#P42">42</a> + Object glass, <a href="#P45">45</a> + Observatories, Berlin, <a href="#P50">50</a> + ---- Copenhagen, <a href="#P50">50</a> + ---- Greenwich, <a href="#P50">50</a> + ---- Mt. Wilson, <a href="#P48">48</a> + ---- Paris, <a href="#P50">50</a> + ---- Pulkowa, <a href="#P50">50</a> + ---- St. Petersburg, <a href="#P50">50</a> + ---- Washington, <a href="#P50">50</a> + ---- Yerkes, <a href="#P47">47</a> + + + "PALLAS" (Minor planet), <a href="#P38">38</a> + Parabola, <a href="#P34">34</a> + "Perseids" (Meteors), <a href="#P80">80</a> + Photography, <a href="#P46">46</a> + Photosphere, <a href="#P69">69</a> + "Pilgrim" star, <a href="#P88">88</a> + Piazzi, <a href="#P38">38</a> + Planets, <a href="#P17">17</a> + Pole of the Heavens, <a href="#P13">13</a> + Pontécoulant, <a href="#P37">37</a> + Precession of the Equinoxes, <a href="#P36">36</a>, <a href="#P83">83</a> + "<i>Principia</i>," <a href="#P36">36</a> + Prominences, <a href="#P73">73</a> + "Ptolemæus" (Lunar crater), <a href="#P60">60</a> + Ptolemy, <a href="#P24">24</a>, <a href="#P81">81</a> + + + RADIANT POINTS, <a href="#P80">80</a> + Radius Vector, <a href="#P28">28</a> + Reflectors, <a href="#P47">47</a> + Refractors, <a href="#P47">47</a> + + + SATURN, <a href="#P18">18</a>, <a href="#P78">78-79</a> + Schiaparelli, <a href="#P63">63</a> + Schwabe, <a href="#P69">69</a> + Seconds of arc, <a href="#P44">44</a> + Sirius, <a href="#P53">53</a> + Solar System, Tables of, <a href="#P56">56-58</a> + Somerville, Mrs., <a href="#P89">89</a> + Spheres, Planetary, <a href="#P21">21</a> + Spörer, <a href="#P71">71</a> + Spörer's Law, <a href="#P71">71</a> + Star catalogues, <a href="#P81">81-83</a> + ---- clusters, <a href="#P88">88</a> + ---- drift, <a href="#P85">85</a> + Stars, fixed, <a href="#P84">84</a> + ---- proper motions of, <a href="#P84">84</a> + Sun, <a href="#P11">11</a>, <a href="#P12">12</a>, <a href="#P14">14</a>, <a href="#P21">21</a>, <a href="#P32">32</a>, <a href="#P67">67-77</a> + ---- distance of, <a href="#P51">51</a> + ---- dials, <a href="#P43">43</a> + Sun spots, <a href="#P69">69</a> + ---- spot maximum, <a href="#P71">71</a> + ---- ---- minimum, <a href="#P71">71</a> + "Sun's Way," <a href="#P85">85</a> + + + TELESCOPE, Invention of, <a href="#P45">45</a> + Transit Circle, <a href="#P82">82</a> + Tycho Brahe, <a href="#P27">27</a>, <a href="#P44">44</a>, <a href="#P88">88</a> + "Tycho" (Lunar crater), <a href="#P59">59</a>, <a href="#P60">60</a>, <a href="#P61">61</a> + + + URANUS, <a href="#P38">38</a>, <a href="#P79">79</a> + + + VARIABLE stars, <a href="#P86">86</a> + ---- ----, Long period, <a href="#P87">87</a> + Venus, <a href="#P18">18</a>, <a href="#P27">27</a>, <a href="#P67">67</a> + "Vesta" (Minor planet), <a href="#P38">38</a> + + + YOUNG, C. A., <a href="#P74">74</a> + + + ZENITH, <a href="#P17">17</a>, <a href="#P88">88</a> + Zodiac, Signs of, <a href="#P14">14</a>, <a href="#P15">15</a>, <a href="#P16">16</a>, <a href="#P43">43</a> +</pre> + +<p><br /><br /><br /></p> + +<p class="t3"> + Printed by BALLANTYNE, HANSON & Co.<br /> + Edinburgh & London +</p> + +<p><br /><br /><br /></p> + +<p class="thought"> +******** +<br /> +</p> + +<p><br /><br /><br /></p> + +<p><a id="chap09"></a></p> + +<p class="t3"> +"We have nothing but the highest praise for these<br /> +little books, and no one who examines them will have<br /> +anything else."—<i>Westminster Gazette</i>, 22nd June 1912. +</p> + +<p><br /></p> + +<p class="t2"> +THE PEOPLE'S BOOKS +</p> + +<p class="t3b"> +THE FIRST NINETY VOLUMES +</p> + +<p class="t3"> +The volumes issued are marked with an asterisk +</p> + +<p><br /></p> + +<p class="t3b"> +SCIENCE +</p> + +<p class="noindent"> + 1. The Foundations of Science . . . By W. C. D. Whetham, M.A., F.R.S.<br /> + 2. Embryology—The Beginnings of Life . . . By Prof. Gerald Leighton, M.D.<br /> + 3. Biology . . . By Prof. W. D. Henderson, M.A.<br /> + 4. Zoology: The Study of Animal Life . . . By Prof. E. W. MacBride,<br /> + M.A., F.R.S.<br /> + 5. Botany; The Modern Study of Plants . . . By M. C. Stopes, D.Sc.,<br /> + Ph.D., F.L.S.<br /> + 6. Bacteriology . . . By W. E. Carnegie Dickson, M.D.<br /> + 7. The Structure of the Earth . . . By Prof. T. G. Bonney, F.R.S.<br /> + 8. Evolution . . . By E. S. Goodrich, M.A., F.R.S.<br /> + 9. Darwin . . . By Prof. W. Garstang, M.A., D.Sc.<br /> + 10. Heredity . . . By J. A. S. Watson, B.Sc.<br /> + 11. Inorganic Chemistry . . . By Prof. E. C. C. Baly, F.R.S.<br /> + 12. Organic Chemistry . . . By Prof. J. B. Cohen, B.Sc., F.R.S.<br /> + 13. The Principles of Electricity . . . By Norman K. Campbell, M.A.<br /> + 14. Radiation . . . By P. Phillips, D.Sc.<br /> + 15. The Science of the Stars . . . By E. W. Maunder, F.R.A.S.<br /> + 16. The Science of Light . . . By P. Phillips, D.Sc.<br /> + 17. Weather Science . . . By R. G. K. Lempfert, M.A.<br /> + 18. Hypnotism and Self-Education . . . By A. M. Hutchison, M.D.<br /> + 19. The Baby: A Mother's Book . . . By a University Woman.<br /> + 20. Youth and Sex—Dangers and Safeguards for Boys and Girls . . .<br /> + By Mary Scharlieb, M.D., M.S., and F. Arthur Sibly, M.A., LL.D.<br /> + 21. Marriage and Motherhood . . . By H. S. Davidson, M.B., F.R.C.S.E.<br /> + 22. Lord Kelvin . . . By A. Russell, M.A., D.Sc., M.I.E.E.<br /> + 23. Huxley . . . By Professor G. Leighton, M.D.<br /> + 24. Sir William Huggins and Spectroscopic Astronomy . . .<br /> + By E. W. Maunder, F.R.A.S., of the Royal Observatory, Greenwich.<br /> + 62. Practical Astronomy . . . By H. Macpherson, Jr., F.R.A.S.<br /> + 63. Aviation . . . By Sydney F. Walker, R.N.<br /> + 64. Navigation . . . By William Hall, R.N., B.A.<br /> + 65. Pond Life . . . By E. C. Ash, M.R.A.C.<br /> + 66. Dietetics . . . By Alex. Bryce, M.D., D.P.H.<br /> +</p> + +<p class="t3b"> +PHILOSOPHY AND RELIGION +</p> + +<p class="noindent"> + 25. The Meaning of Philosophy . . . By Prof. A. E. Taylor, M.A., F.B.A.<br /> + 26. Henri Bergson . . . By H. Wildon Carr, Litt.D.<br /> + 27. Psychology . . . By H. J. Watt, M.A., Ph.D., D.Phil.<br /> + 28. Ethics . . . By Canon Rashdall, D.Litt., F.B.A.<br /> + 29. Kant's Philosophy . . . By A. D. Lindsay, M.A.<br /> + 30. The Teaching of Plato . . . By A. D. Lindsay, M.A.<br /> + 67. Aristotle . . . By Prof. A. E. Taylor, M.A., F.B.A.<br /> + 68. Friedrich Nietzsche . . . By M. A. Mügge.<br /> + 69. Eucken: A Philosophy of Life . . . By A. J. Jones, M.A., B.Sc., Ph.D.<br /> + 70. The Experimental Psychology of Beauty . . . By C. W. Valentine,<br /> + B.A., D.Phil.<br /> + 71. The Problem of Truth . . . By H. Wildon Carr, Litt.D.<br /> + 31. Buddhism . . . By Prof. T. W. Rhys Davids, M.A., F.B.A.<br /> + 32. Roman Catholicism . . . By H. B. Coxon. Preface, Mgr. R. H. Benson.<br /> + 33. The Oxford Movement . . . By Wilfrid Ward.<br /> + 34. The Bible and Criticism . . . By W. H. Bennett, D.D., Litt.P.,<br /> + and W. F. Adeney, D.D.<br /> + 35. Cardinal Newman . . . By Wilfrid Meynell.<br /> + 72. The Church of England . . . By Rev. Canon Masterman.<br /> + 73. Anglo-Catholicism . . . By A. E. Manning Foster.<br /> + 74. The Free Churches . . . By Rev. Edward Shillito, M.A.<br /> + 75. Judaism . . . By Ephraim Levine, M.A.<br /> + 76. Theosophy . . . By Annie Besant.<br /> +</p> + +<p class="t3b"> +HISTORY +</p> + +<p class="noindent"> + 36. The Growth of Freedom . . . By H. W. Nevinson.<br /> + 37. Bismarck and the Origin of the German Empire . . .<br /> + By Professor F. M. Powicke.<br /> + 38. Oliver Cromwell . . . By Hilda Johnstone, M.A.<br /> + 39. Mary Queen of Scots . . . By E. O'Neill, M.A.<br /> + 40. Cecil John Rhodes, 1853-1902 . . . By Ian D. Colvin.<br /> + 41. Julius Cæsar . . . By Hilary Hardinge.<br /> + 42. England in the Making . . . By Prof. F. J. C. Hearnshaw, M.A., LL.D.<br /> + 43. England in the Middle Ages . . . By E. O'Neill, M.A.<br /> + 44. The Monarchy and the People . . . By W. T. Waugh, M.A.<br /> + 45. The Industrial Revolution . . . By Arthur Jones, M.A.<br /> + 46. Empire and Democracy . . . By G. S. Veitch, M.A., Litt.D.<br /> + 61. Home Rule . . . By L. G. Redmond Howard.<br /> + Preface by Robert Harcourt, M.P.<br /> + 77. Nelson . . . By H. W. Wilson.<br /> + 78. Wellington and Waterloo . . . By Major G. W. Redway.<br /> +</p> + +<p class="t3b"> +SOCIAL AND ECONOMIC +</p> + +<p class="noindent"> + 47. Women's Suffrage . . . By M. G. Fawcett, LL.D.<br /> + 48. The Working of the British System<br /> + of Government to-day . . . By Prof. Ramsay Muir, M.A.<br /> + 49. An Introduction to Economic Science . . . By Prof H. O. Meredith. M.A.<br /> + 50. Socialism . . . By B. B. Kirkman, B.A.<br /> + 79. Mediæval Socialism . . . By Bede Jarrett, O.P., M.A.<br /> + 80. Syndicalism . . . By J. H. Harley, M.A.<br /> + 81. Labour and Wages . . . By H. M. Hallsworth, M.A., B.Sc.<br /> + 82. Co-operation . . . By Joseph Clayton.<br /> + 83. Insurance as a Means of Investment . . . By W. A. Robertson, F.F.A.<br /> + 92. The Training of the Child . . . By G. Spiller<br /> +</p> + +<p class="t3b"> +LETTERS +</p> + +<p class="noindent"> + 51. Shakespeare . . . By Prof. C. H. Herford, Litt.D.<br /> + 52. Wordsworth . . . By Rosaline Masson.<br /> + 53. Pure Gold—A Choice of Lyrics and Sonnets . . . by H. C. O'Neill<br /> + 54. Francis Bacon . . . By Prof. A. R. Skemp, M.A.<br /> + 55. The Brontës . . . By Flora Masson.<br /> + 56. Carlyle . . . By L. MacLean Watt.<br /> + 57. Dante . . . By A. G. Ferrers Howell.<br /> + 58. Ruskin . . . By A. Blyth Webster, M.A.<br /> + 59. Common Faults in Writing English . . . By Prof. A. R. Skemp, M.A.<br /> + 60. A Dictionary of Synonyms . . . By Austin K. Gray, B.A.<br /> + 84. Classical Dictionary . . . By Miss A. E. Stirling<br /> + 85. A History of English Literature . . . By A. Compton-Rickett, LL.D.<br /> + 86. Browning . . . By Prof. A. R. Skemp, M.A.<br /> + 87. Charles Lamb . . . By Flora Masson.<br /> + 88. Goethe . . . By Prof. C. H. Herford, Litt.D.<br /> + 89. Balzac . . . By Frank Harris<br /> + 90. Rousseau . . . By F. B. Kirkman, B.A.<br /> + 91. Ibsen . . . By Hilary Hardinge.<br /> + 93. Tennyson . . . By Aaron Watson<br /> +</p> + +<p><br /><br /></p> + +<p> +LONDON AND EDINBURGH: T. C. & E. C. JACK<br /> +NEW YORK: DODGE PUBLISHING CO. +</p> + +<p><br /><br /><br /><br /></p> + + + + + + + + +<pre> + + + + + +End of Project Gutenberg's The Science of the Stars, by E. 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