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Les cartes, planches, tableaux, etc., peuvent dtre filmds d dos taux de rdduction diffdrents. Lorsque le document est trop grand pour dtre reproduit en un seul cliche, il est filmd d partir de Tangle supdrietir gauche, de gauche d droito, et de haut en bas, ^n prenant le nombre d'images ndcessaire. Les diagrammes suivants illustrent la m6thode. rrata :o pelure, 1 d □ 32X 1 2 3 1 2 3 4 5 6 SC] I SHHMP^^ini \ 7 "1 SCIENCE PRIMERS, edm by Professors Huxley, Roscoe, and * Balfour Stewart. ASTRONOMY. 4 ~t , t i A Ltiiuur Crater. 4 ,. ■? I I ^timcz mmtxB, ASTRONOMY. BY J. NORMAN LOCKYER, F.R.S. Correspondent of the Institute qf France, Author of ''Elementary Lessons in Astronomy^' <&-«•. WITH ILLUSTRATIONS. SECOND EDITION. AMES CAMPBELL & SON. 1876* 17:4^ kight of TranslaHon and ReprodurHon is Reserved.'] 4«ti.w4» tt^4^ii'»^* ^ A ^ «# tViA Parliament of Canada, in the year one EnteredaccordtagtotheA^^^^ *^Tsoi! to S& of the Miifister'of Agriculture. Huimit, Boss ft Co. Printers, TonONTO. PREFACE. In writing this little book I have endeavoured first to help the reader, by means of simple ex- periments, to form true ideas of the motions of the heavenly bodies; and then to give a sketch of the Earth's place in Nature, and of the use made of the heavenly bodies for Geographical purposes. 1 I have been much aided by my friend, Mr. G. M. Seabroke of the Temple Observatory, Rugby, to whom my acknowledgments are due. ^ J. N. L. ii ■*« \ CONTENTS. ■ PACK Introduction ..•..,. i * C. The Earth and its Motions. SECT. I. — The Earth is round . » . 2. — The Earth is very large ^ 3-— The Earth is not at rest jq 4.— The Earth spins or rotates like a top ... 13 5'— The Earth rotates once in a day jc 6. -^The rotation of the Earth is not its only motion 19 7-— The Earth travels round the Sun once in a year 22 8.— The two motions of the Earth are not in the same plane 23 9.— Why the Days and Nights are unequal ... 26 10.— The Seasons depend upon the difference in the lengths of the Day and Night 33 II.— .Whythe movements of the Sunand Stars appear different in different parts of the Earth . . 35 II. The Moon and its Motions. l.~The Moon travels among the Stars .... 40 2.— The Moon changes h^ form ^ 3.— How the Moon causes Eclipses ..... 45 4.— What the Moon is like ^ ' ! 53 CONTENTS. III. Thk Solar System. SECT rAGB I.— How bodidB like theEarth,neaTer the Sun, would appear to us 5^ a.— How bodies like the Earth, further off from the Sun, would appear to us . 5® 3.— Are there such bodies ?— The Planets ... 6c 4.— The Interior Planets 62 5.— The Exterior Planets ^^ d— Comets, Meteorites, and Falling Stars ... 77 IV. The Sun— The Nearest Star. I.—The influence of the Sun in the Solar System . 81 2.— The Heat, Light, Size, and Distance of the Sun %2 3.— "What the Sun is like . 4. — Sun-spots ...•.» 5.— The Sun's Atmosphere . . 6.- What the Sun is made of . 7,— The Sun is the nearest Star. 83 84 86 87 88 V. The Stars and Nebula I.— -The Stars are distant Suns . . . 2.— The brightness of the Stars. . • 3. ^The Constellations 4.— Apparent movements of the Stars c, ^Real movements of Stars . • • 6.— Multiple Stars 7. Clusters and Nebulae 8.— The nature of Stars and Nebulae . . 89 . 89 . 91 . 93 . 96 . 96 • 97 . 100 * CONTENTS. XI VI. How THE Positions of the Heavenly Bodies are Determined, and the Use that is Made op i;: Them. . ■ . . ■■ '■ ^ . ., V, ,;^, ^; ' .;^_ SECT. ''■.'-■ • , PACK I, — Recapitulation — Star Maps ••••,••• 102 2. — Polar Distance 1 • . . 103 3. — Polar Distance is not sufficient 104 4. — Right Ascension . . . ' # • • • . • .106 5. — Recapitulation . . . , *. . . ' • • • ,108 6. —The Latitude of Places on the Earth . , * . 108 7. — The Longitude of Places on the Earth , • , in VII. Why the Motions of the Heavenly Bodies are so Regular. I. — "What Weight is • , • . 114 2. — Gravity Decreased with Distance 117 ^ — How this explains the Moon's path round the Earth. ......<•.•• IiS 4.— The Attraccio.i of Gravitation .••».• 120 Ml . Jl i f J , .,<\ LIST OF ILLUSTRATIONS. PAGB Plate I.— Frontispiece. A Lunar Crater . • . To face Title ^^ 2.— The Solar Systen. Behveen 60 & 6i Pig. I. —How ships become visible and disappear at sea . 4 „ 2,— Explanatory of the above . 5 ^^ 3. -^Diagram shtwing how, when we suppose the earth is round, we explain that ships at sea appear as they do . . 6 ^^ 4. — Diagram explaining how it is that the higher we go the further we can see 7 „ 5.— Diagram showing that the larger the earth is sup- posed to be, the further removed from us is the place at which the sky appears to touch the earth. , . . ^ „ 6.— Explanation of sun-rise and sun-set, and star- rise and star-set ^^ „ 7.— -The same -••••»..• 12 „ 8.— A top spinning 14 „ 9.— The direction of the earth's spin 14 „ 10.— Experiment to illustrate the spinning of the earth, as causing day and night • 1 5 „ II.— Explanation of the earth's motion round the sun 19 „ 12. — ^Thfc plane of the ecliptic 24 „ 13.— 1 wo planes cutting each other at right angles . 25 ,, 14.--TW0 planes cutting each other obl'quely . . . aj s XIV LIST OF ILLUSTRATIONS. PAGB , Mi 4ii ^ig' IS-- „ i6.- » 17- 18.- » » >» 19.- „ 20.- „ 21.- 26 29 30 32 34 22. — 23. 24 25- S6. 27. 28. „ 29- >» 30- »» 31. »f 32. >» 33 -Earth with axis of rotation inclined to plane of ecliptic • • • • • • • ^ * \, • * * * ■ * The Earth, as seen from the Sun at the Summer Solstice, June 22 (noon at London) .... •The Earth, as seen from the Sun at the Winter Solstice, Dec. 22 (noon at London) . ;,;'», The Earth, as seen from ihe Sun at the Vernal Equinox, March 22 (noon at London) ... The Earth, as seen from the Sun at the Autumnal Equinox, Stpt. 22 (noon at London) pj|^ ^ «^ Explanation of the Seasons . • »>• . • . The Pole Star and the Constellation of the Great Bear in four different position:^, after intervals of six hours, showing how the Great Bear appears to travel round the Pole Star H The Moon's motion round the Earth . ^ V -Total EcUpse of the Sun . fsrR tes^J^t; -Annular Eclipse of the Sun . . • • \ -Eclipse of the Moon » . . ■■•, . . , -Showing the inclination of the Moon's orbit to the plane of the ecliptic 50 -Division of the Circle into degrees ..... 51 -Diagram illustrating the motions and appearances of a body between us and the Sun .... —Diagram illustrating the motion of a body travel- ling round the sun outside the orbit of the earth —Venus, showing the marking's on its surface . . -Apparent size of Venus, at its least, mean, and . greatest distance from the Earth ..... 65 —Mars, showing snow cap at the pole, and the lands and seas 68 —Mars. View of another part of the planet . . 69 p*** 36 '4 , 43 k • 46 i • 47 . . 48 57 59 64 PAGB leof * « 26 mer 1 • 29 nter 30 mal • • 31 mal r- •-. 32 » • 34 reat vals ?ear "" j'-^*' . 36 » • 43 > • 46 1 • 47 1 « 48 : to > • 50 > • 51 ices • 57 vel- irth 59 • 64 and . • 65 the • 68 « 69 \ LIST OF ILLUSTRATIONS. VI Fig. 34-- 1* 35." >f 36.- )» 37.- » 38.- »» 39-- f) 40.- >» 41.- ») 42. >» 43.- » 44.- »» 45-- *> 46. >> 47. >f 43. Jar?' • • PACK -Jupiter, showing the cloud belts 7 1 -Diagram explaining the eclipses, occultations, and transits of Jupiter's satellites -Saturn and his rings . . • • -General view of a Comet .••••••• -Head and Envelopes of a Comet -How the size of the Sun is determihed . . . -A Sun-spot • -Explanation of the appearances presented by Sun-spots ..•• -The Sun's coronal atmosphe»"e ••••<.. -Orbit of a Double Star •••••#•• -The Cluster in Hercules • • -The Great Nebula in Orion ,...#.. -How to define the position of anything . • . —How the positions of stars are stated • • • . -Diagram showing the fall of the Moon towards 72 74 77 79 83 85 86 87 97 98 99 104 106 the Earth j<|^ \:ii8 ■** • 119 : *■-, Aj- jJi-' x-ii-f ;■ -^ -! ' 3ft' '^"mmtmB ■■•-f^'i :, ti '"?|S q SCIENCE PRIMERS. ASTRONOMY. INTRODUCTION. 1. Everyone who is going to read this book knows what a school-room or school-house is. Now suppose it had windows that you could not see through, and that you never went out of it: then you would think, perhaps, that the school-house was all the world. But you know better. You know that your school-house is only one house out of many, perhaps in the same street, or at all events in the same parish, whether in the country or the town; most of you even will have walked or ridden into the Parishes which lie round the one in which you live. 2. If my reader lives in London, he will have done more than this, perhaps, for if he has crossed one of the bridges over the Thames he will have gone from one County to another (a county being a collection of parishes as a street is a collection of houses), for the River Thames divides the counties of Middlesex and Surrey. 3. Just as a county is a collection of parishes, so B SCIEME PRIMERS, '>: I- ii ■1 i the Country of England, or of Scotland, or of Ireland, or of Wales, is a collection of counties ; these four Countries forming the United Kingdom of Great Britain and Ireland. Now wherever you are, whether in a town or village school, whether in the United Kingdom, America, Australia, or India, before you read the next paragraph, write down the ^p:yri:MX}-^ School, Street, Parish, County, Country, Kingdom, V' AjPi'J , - ... t'lf' \ in which you are, *f^ and this will show you that your school house is only a very little speck on the broad lands which togethei form the United Kingdom, or whatever kingdom you happen to be in. 4. Although you may not have gone to France 01 Germany, you have heard of those places. What are they? Well, the United Kingdom, France, Germany, Russia, Italy, Turkey, and other countries, form the continent of Europe, a continent being a collection of countries, as a country is a collection of counties^ and as a county is a collection of parishes. 5. You may also have heard of America, Asia, Africa, and Australia, as well as of Europe; nay, you may even be living in one of these, which, like Europe, are Continents. 6. Now these continents are the largest stretches of dry land on the surface of The Earth, the surface being partly water and partly land. T ASTRONOMY. 7. I have next to tell you that the earth, taken as a whole, is a body which astronomers call a planet: what this is you will lesm by and by. Before going further, write down as before, the School, \ Street, Parish, ^ ]"* \ in which you are. Country, ( ,,^,.J, . Kingdom, Continent, Planet, / 8. Some of you may think that I have made a mistake, and am going to write a book on Geography instead of Astronomy. I have not made a mistake. I want to show you that where Astronomy leaves off Geography begins ; that just as the shape, and size, and position of your school, which is a little speck on the planet on which we dwell, called the earth, can be stated, and just as men by tvc veiling, can find out lands on the earth, far away from your school, and tell us all about them, so are the shape, size, and position of the earth itself, among all the bodies in the skies, known, and its relation to them can be made clear to you. This is what I have to try to do, and if I can manage to do it, then you will understand better when you come to read about the surface of the earth. ■^■^^^iwrr-^-Tvm-:. ^mU^r'^S^rrTx^f^^fj----^ |;-7| B 2 SCIENCE PRIMERS. [|I I.— THE EARTH AND ITS MOTIONS. I I.— THE EARTH IS ROUND. 9. Now I have said that we are on a planet which we call The Earth, but what sort of thing is it ? Is it flat or curved, square or round ? How are we to find this out ? If you look in any direction, if you are in a hilly country, you see hills and valleys ; and if you walk over these hills, more hills are generally found rising U;^ which limit the view to a few miles ; if you are in a flat country, the trees and shrubs appear to meet the sky in every direction around you. We may travel to any place we like, still there is this line where the surface of the earth and the sky meet, so that for aught we could tell to the contrary in this Fig. X.— How the ships appear and disappear at sea. way, the earth might be a nearly flat surface of large extent. ASTRONOMY. 16. But let us try where there are no rocks or trees, where the surface of the earth is unbroken and smooth ; let us try the surface of the sea. Watch the ships in the distance just coming into view, and you will find that only their masts are visible ; as they approach, more and more of the hull appears, until it is quite ol- house, and other pins to picture to you the trees and homes round it i 26. You will see at once that whether the worsted ball or the orange is at rest or in motion, the positions of the pins with regard to each other will not change. 27. How, then, are we to settle the question ? By looking at something not on the earth. Go out en a clear evening, and look in the east (every bey and girl should know where the north, south, east, and west points are) : you will see the stars rising higher and higher above the edge of the earth, that is, the line where the earth's surface and the sky meet, which we must henceforth call the horizon. Those in the west will be r;radually disappearing just in the same way ; the moon also follows their example. In ASTRONOMY. \\ the day-time we iind that the su^ rises in the east and sets in the west, in exactly the same manner. 28. Here there is proof positive that while the houses and trees on the earth's surface do not move with regard to each other, the sun, stars, and moon, which are not on the earth's surface, do move, or appear to move, with regard to the earth. 29. Now let us think about this. What do we mean when we say that a star or the sun rises and sets ? We mean that it is just passing either up or down over the edge of the earth seen from the place where we are ; the sun or star in fact does, or appears to do, just what the ships that we referred to in par 10 did. The ball of worsted or the orange should make this \ Fig. 6, — Explanation of sun-rise and sun-set, and Star-rise and star-set. quite clear. Put it on the middle of a table, and stick a pin into its side, the pin's head to represent your eye. Now imagine yourself to be the sun or a star, and walk round the table as represented in Fig. 6, keeping your eye on a level with the pin ; at one point the pin will be seen just rising from the edge of the ball ; you are playing the part of a rising sun or star, to your own eye represented by .the pin's 13 SCIENCE PRIMERS. [% in. head: at another point in your journey round the table the pin's head will disappear, and at last will be hidden by the edge of the balL Here you are playing the part of a setting sun or star, «;dpposing the earth to be at rest. 30. Now sit down and get someone to turn the ball of worsted round for you, keeping the pin's head always at the same distance above the table. In this case, the motion of the ball, while you are at rest, will give rise to the same appearances as those you saw when the ball was at rest, and you walked round it Fig- ?• — Diagram explaining Fig. 6 ; with the direction of motion indicated a body at A is setting, at B is rising, and at C is overhead. 31. Hence the appearances connected with the rising and setting of the sun and stars, may be due either to our earth being at rest and the sun and stars travelling round it, or the earth itself turning round, while the sun and stars are at rest. The ancients thought that the earth was at rest, and that the sun and stars travelled round it. But we now know that it is the earth which moves. ASTRONOMY, n be S IV.— THE EARTH SPINS OR ROTATES LIKE , A TOP. 32. You have then to take it as proved that the earth moves, and that the seeming movements of the sun, moon, and stars, as they travel from east to west, the sun by day, and the moon and stars by night, are not real movements, but are apparent movements only, brought about by the actual movem( t of the earth. 33. How then does the round earth move? Let us think a little. Have we any familiar example of such apparent movement of objects afc rest brought about by our own movement? Yes, certainly we have. You ^W. all at once think how, when you are sitting in a railway-carriage, all the objects, trees, houses and what not, that you can see out of the window and are really at rest, appear to fly past you as if you were at rest. Further, they appear to sweep past you in the direction exactly opposite to the one in which you are going. 34. So far so good. Now will it do to apply this reasoning at once to the earth and stars, to imagine that the whole earth is really moving rapidly from the point that we call West towards the East, and is rushing rapidly past the sun and moon and stars? and that this is the reason they appear to move from East to West? 35. You will at once see that it will not do to reason thus, because we should thus never see the same sun and moon and stars again. 36. How then can we explain the facts ? We can imagine that the earth spins round as a top 14 SCIENCE PRIMERS, t§iv. does, so that every morning every boy and girl, whether living in England, or America, or Australia, Fig. 8. — A top spinning. Em or India, sees the same sun rise, and every evening sees the same sun set. 37. It is in fact because the earth does^ttiiSi in this way that we haire morning and evening at all, and day Fig. 9. — The direction of the earth's spin. and night are the best proofs that the earth does really spin as I state that it does. ASTRONOMY, 15 Tfi. And because the sun seems to rise in the East and set in the West, the earth really spins in the opposite direction, that is, from West to East. 39. Now get a common school globe. Set it spin- ning as you would a top ; that is, let the axis be upright as a top's is. Which way is it to turn? With your right hand push the right-hand surface of the globe away from you. The globe then represents the direction in which the real earth turns. § v.— THE EARTH ROTATES ONCE IN A DAY. 40. Take an orange, to represent the earth, into a dark room, with a lamp to represent the sun; stick a knitting needle through the centre of the orange, and then upright into a pincushion having also stuck a small pin as far as it will go into the orange, so that Fic xar-Experiment to illustrate the spinning of the earth, as causing uay and night. , ■B its head shall represent an observer on the earth. Twist the needle round, and so make the orange turn /i ■ ^ i6 SCIENCE PRIMERS. [§v. round slowly, in the contrary direction to that in which the hands of a watch move, as in Fig. 9. 41. Examine what happens. First, there will be two points on the orange through which the knitting needle passes, which do not move, and these are called the poles, the one at the top we will call the north pole, and the bottom one the south pole, the line joining the poles we will call the axis ; this is repre- sented by our needle. Draw a circle round the middle of the orange, everywhere at the same distance from the poles, or just where we should cut the peel if we were going to cut a lily or other similar device from the fruit: this line we will call the equator. Let the pin's head'be near this line and opposite the lamp representing the sun. One half of the orange will, of course, be lighted up by the lamp, representing day, and the other half dark, representing night, yitf 42. Now twist the knitting needle slowly, and you will see that the pin's head, instead of being exactly in the middle of the half of the orange first lit up by the lamp, will, when the orange has turned through a quarter of a circle, be just visible at the edge of the lighted portion ; a slight turn more, and no light reaches it, — ^the lamp has set. Turr. the orange another quarter of a circle, and you find the pin's head is in the centre of the dark side, with its head turned exactly opposite to the lamp \ another quarter's turn, and the pin's head is just coming into the lamp- light — the lamp is rising; a quarter of a turn more, and the orange has turned round once, and the lamp is again shining directly overhead as at first 43. The lamp has therefore apparently passed from over the pin's head, set, and risen, and come to the ASTRONOMY, 17 lit 1^- same place again, simply by turning the orange round. ^^ 44. So with the earth, it rotates as the orange has done, in the same way, round, not a knitting-needle, but an imaginary axis, passing through its poles. 45. Day and night are thus caused, and as the sun appears to take twenty-four hours to move from where it is at any time to the same place again the next day, we learn that the earth actually takes twenty- four hours to turn once on its axis. (Par. 41.) j 10 46. It is time now that we made use again of an ordinary school-globe. Get one of these and place the lamp a few feet from it, on a level with its centre. Let the axis of the globe be upright, and make the globe turn round. Whether it is allowed to remain at rest or is sent spinning round rapidly, the half of it next the lamp will be illuminated, and the other half away from the lamp will be in shade. When it is at rest, the places on one side remain in the light, while ihose on the opposite side remain in the dark. As you turn it round, each place in succession is brought round to the light, and carried on into the shade again. And while the lamp remains unmoved, the rotation of the globe brings alternate light and dark- ness to each part of its surface. 47. Now, instead of the little school-globe, imagine the earth, and in place of the feeble lamp, the great sun, and you will see how the rotation or spinning round of the earth on its axis must bring alternate light and darkness to every country^ \ 48. You must not suppose that there is any actual rod passing through the earth to represent our knitting- needle and the steel rod of the school-globe, to form t i8 SCIENCE PRIMERS, Bv. the axis round which it turns. The axis is only an imaginary line, and the two opposite points where it reaches the surface, and where the ends of the rod would come out were the axis an actual visible thing, are still called the North Pole and the South Pole, both on the globe and on the earth itself. 49. The earth spins then round this axis once in every twenty-foui hours. All this time the sun is shining steadily and fixedly in the sky. But only those parts of the earth can catch his light which happen at any moment to be on the side turned towards him. There must always be a bright side and a dark side, juLt as there was a bright side and a dark side, when you placed first the orange and then the globe oppo- site to the lamp. Now you can easily see that if there were no motion in the earth, half of its surface would never see the light at all, while the other half would never be in darkness. But since it rotates, every part is alternately in sunlight and in darkness. When we are catching the sun's light, we have Day ; when we are on the dark side, we have Night. 50. The sun seems to move from east to west. The real movement of the earth, is, for a reason which has been stated in par. 38, just the reverse of this, viz. from west to east. In the morning we are carried round into the sunlight, which appears in the east. Gradu^ly the sun seems to climb the sky until he appears highest at noon, and gradually he sinks again to set in the west, as the earth in its rotation carries us round once more out of the light. At night we trace the movement of the earth by the way in which the stars one by one rise and set, as die sun rises and sets in the daytime. m ASTRONOMY, 19 VI.— THE ROTATION OF THE EARTH IS NOT ITS ONLY MOTION. 51. You are now probably convinced of these facts First, that the earth is a globe. Secondly, that the earth spins like a top. WALL A TABLE t I r- r O WAU e Fig. II.— Explanation of the Earth's motion round the Sun. And lastly, that without this spinning there could T)e no day and night, so that the regular succession of day and night is caused by this spinning. / c 2 20 SCIENCE PRIMERS, [§VI. 52. Here then we have fairly proved that the earth has one motion. Now the question comes, has it more than one? How shall we settle this? Well, first of all let us see if this one motion will account for all the things we see. 53. To do this we must again have our globe and orange, and imagine them in a room with many pic- tures on the walls. You wonder what pictures have to do with it ? Well, I want the pictures to represent the stars in the sky. There are stars all round the part of space in which the earth and the sun are, only we cannot see them in the daytime, because the sun is so bright. So that if you have pictures all round the globe and orange they will represent the stars. Of course there should be pictures on the ceiling and floor too, but we will content ourselves by imagining them to be there as well 54. Now imagine the globe at rest and the orange at rest. Do not turn it round even* Then, as we have already seen, if we imagine the orange to represent the earth, and the lamp to represent the sun, that part of the orange turned to the sun, represented by th6 lamp, will have per- petual day, and will always see the same ] « n 1 in the same place \ from that part of it turned away from the sun the same \ Jl \ will always be visible in the same place. From the parts of the I arth I ^^^^ *^^ boundary of light and shade . f sun, stars ) •« i. r *«> ^"^ i lamp, pictures } '^ ^ ^<^' "^"^ *P' ASTRONOMY. 21 patently near the horizon (par. 27) in the same place. 55. Now stick a pin in the equator (par. 41) of the orange up to the head, to represent an observer on the earth, turn the orange round to represent the spinning or rotation, as we must now call it, of the earth, and mark that whenever the observer represented by the pin's head is in the middle of the lighted-up half, the part exactly opposite is in the middle of the dark half, and that half a turn of the orange brings the pin's head from the middle of the lighted-up to the middle of the dark portion. Now these two positions — namely, the middle of the lighted-up half and the middle of the dark half — represent nearly enough for our present purpose the position with regard to the sun which an observer is made to occupy at midday and midnight by the earth's rotation. 56. You will see in a moment, therefore, that if neither the sun nor the earth move from their places, we shall always see one particular set of stars at mid- night, another particular set at sunrise, and another particular set at sunset. 57. Think this well over and reason it out with the pictures, for it Is a very important point for you to understand clearly. 58. Now, is it a fact that we always do see the same stars at midnight? No. Then what are the facts ? (i). If we view the stars at midnight in summer, and again at the same time in winter, we see diffident stars. Here then is a great change in six months. (2). If we view the stars for many nights in succes- aa SCIENCE PRIMERS. [% VII. sion at midnight, we find them gradually falling away to the west. Here is a slight change in a few days. (3). After the lapse of a year the same stars are visible at midnight. 59. No V move the orange round the lamp in the same direction as the earth rotates, and vou will se ? at once thstt this explains all the facts. 60. In Fig. II. I have given a drawing of the lamp, orange, table, and room, as you would see them from above. First consider the orange at A» Then at mid- night the observer on the dark side would see the stars opposite to the sun, the pictures on wall A : at B, at midnight he would see the stars opposite the sun, now represented by the pictures on wall B ; and therefore no longer the same stars as were seen before. So on with the positions at C and Z>. ' -^^^ 61. I must next point out to you that the same effects would be produced as those we see and have thus accounted for, by supposing the sun to travel round the earth in the opposite direction. But we know that the earth really travels round the sun, and not the sun round the earth. -u- § VII.— THE EARTH TRAVELS ROUND THE SUN ONCE III A YEAR. 62. The earth then not only rotates on its axis once a day, but travels round the sun. In this way we have accounted for the fact that as seen at midnight, or at the Same nour every night from any part of the earth, whether England, America, Australia, or ftidia, the stars visible are continually changing. We have found also that tbey change very little in & few ASTRONOMY. 23 nights, very much in six months, and that after twelve months the same stars again appear in the same places. 63. Now my reader should ag^in go to his lamp and orange, and he will find that precisely as the earth spins in a day, so it goes round the sun in a year. 64. For it is clear that if for instance the journey only required six months, then in six months* the same stars would be visible at midnight, and so on for any other period you might choose to suggest. Here then we have the origin of the year, which is the time the earth requires to get back to the same place in its path round the sun. § VIII.— THE TWO MOTIONS OF THE EARTH ARE NOT IK THE SAME PLANE. ' 65 i *' ilow does the earth travel round the sun ? does it -jerk, or go up and down, or always smoothly and right on, keeping the same level ? " some of you m^y ask, I answer, the earth travels smoothly, and always keeps the same level ; as horses do, galloping round a very level race-course. To picture this more exactly^ imagine a very large ocean with the sun and earth floating on it up to their middles, then imagine the earth to travel thus round the sun once a year in a nearly circular path, that is, always keeping about the same distance from the sun. 66. Now get five balls, one larger than the others, to represent the sun ; weight them so that they sink up to their middles, and then put them in a tub of lya^er as shown in Fig. ij?, 24 SCIENCE PRIMERS, [§ VIII. 67. We have now a representation of the sun, and of the earth in four parts of its annual journey. What I want you to understand is that the motion of the earth is not only smooth, but that its motion is in the same plane, a plane being a level surface re- presented by a sheet of cardboard or the surface of the water in the tub : and next that this plane in 7S^- Fig. 12.— The plane of the Ecliptic. which the earth nK)Ves ^sses" tft^gh the cehtM15f ' tl* e sun and earth, as the centres of the balls will be on a level with the water if you have weighted them properly. Further let me call the plane represented by the level surface of the water the Plane of the Ecliptic. 68. Here then is defined the plane of the earth's motion yearly round the sun; this plane of the ecliptic is the earth's race-course. What is the rela- tionship of this to the plane of the earth's daily motion round its axis ? 69. Now it is clear that if the earth's axis is sup- posed to be upright with regard to the plane of the ASTRONOMY, 9$ \ ecliptic, or to form a " right angle '* with it, the plane of the earth's spin will be the same as the plane of the earth's motion round the sun. This is the state of things represented in Fig. 1 2. 70. But are these planes the same? Let us sup- pose them to be so. Stick a pin into one of the smaller balls, make the ball spin uprightly like a hum- ming top, and it will represent the earth as it travels round the sun, and you will find that on this sup- is^* • Fig. i3.~Two planes cutting each other at right angles. position, the days will always be of the same length, because the boundary of light and darhaess would i ^di 'to, mw Fig. X4.— Two planes cutting each other obliquely. pass through the two poles, so that each part of the §:pth's surface would be an equal time in the lighted 26 SCIENCE PRIMERS, [§ix. up, and in the dark, half, if the motion of rotation were uniform. But the days are not all of the same length; in winter in England they are short, and the nights are long; and in summer the days are long, and the nights are short ; and, further, while it is Christmas here in England and America it is summer in Australia. ^ .^ . ^ ^ 1a;? .-,,->= 71. So then the planes '6ftKe''tw3iirtMoHsfcaftnot be coincident; but we can explain all the facts by assuming them to be inclined to each other as shown in Fig. 14, so that the earth's axis in its journey round the sun is really represented by the little balls in Fig. 15, in which they no longer spin upright as in Fig. 12, but their axes are inclined. - • ;^^ct-^ . . *^,^,. rt'Titiif ft , ''fH^i^^S rfi ■^0 fi^ff;? G\ Mm Fig. 15. — Earth with inclined axis of rotation. ^^ fj^^^iff j § IX.— WHY THE DAYS AND NIGHTS ARE UNEQUAL. 72. We can now leave the tub, and come back to the lamp and orange, remembering that the knitting- needle, must no longer be upright as we allowed it ASTRONOMY. . t. 27 rISvi to be in Fig. lo, and that the plane of the ecliptic is represented by the horizontal plane in which lies the line joining the centre of the lamp and the centre of the orange. 73. We have before accounted for day and night, now let us see if we can explain why they differ in length, at different seasons of the year. Place the lamp as before on a table in the middle of the room, and support the orange at the same height as before, inclining the upper end of the knitting-needle a little way from the lamp. Let us call the upper pole the north pole. 74. Now turn the orange round, and you will see that the light never shines on the part of the orange near the north pole, and always shines on a part round the south pole, however rapidly you turn the orange ; but that, as before, parts near the equator alternately become lighted and darkened. Now stick a pin in , the orange, to represent an observer near the north pole, and again twist the orange, and you will see that he never gets into tjie light region ; stick it near the south pole, and here he will always see the lamp, so that; with the earth in this position with regard to the sun, to a person at the north *pole it is always night, and at the other pole always day. 75. Again stick the pin in the orange, about half-way between the equator and the north pole, and twist the orange, and you will see that, as it travels round with the orange, it has a much longer journey round on the dark side of the orange than it has on the light side. At this point, therefore, the night is much longer than _ the day, and you will see that the nearer you place the pin tQ tb? npr^h pQJe, th^ §b9f t^r i^ili 1?^ its period 88 SCIENCE PRIMERS. [§ix. of illumination, till it gets so far north as never to be illuminated at all. 76. On the other hand, the nearer you place the pin to the equator in the northern half of the orange the longer it is lighted, or the days become longer and the nights shorter, till on the equator the journey in the light is just equal to that in the dark. 77. Exactly the reverse takes place on the south side of the equator; the further you place the pin towards the south pole, the longer will its journeys in the light become, till near the pole it never passes into darkness. - , ^ > 78. Now if you rease the inclination of the knit- ting-needle away from the lamp, you will see that the days and nights become more and more unequal at any place where you choose to place the pin, except at the equator, and the less you incline it from the lamp the less is the inequality, so that when it is upright, day and night are equal all over the orange. Now you all kliow that England is on the north side of the equator, about half-way between the equator and pole, but somewhat nearer the pole than the equator ; and you also know th^t in winter the days are much shorter than the nights, and we at once therefore account for this by supposing the axis of the earth to be tipped in the same manner and direction as that of the orange, so that the orange in the case just men- tioned represents the earth in the winter. 79. It is, however, not always winter with us, and following winter comes spring, when the days and nights are equal in length on March 22 ; then comes summer in three months more, when the days are longer tba» th9 'o^^^^ \ JHst |h? reverse of what hap- .'1 03' m to •eg A uB ':^:^'*\U' ir. 'O j,. ,.^ ASTRONOMY, it\'.=r-->-_-~ f.^ J «» ■ 29 pens in winter. In autumn, on September 22, the days and nights are again equal. How can we ac- count for this? Let us consider, and return to our orange; we might try to explain it, by tipping the orange less and less till the axis is uprignt to re- present spring, and then tip it towards the lamp to *iG. io.— The Earth, as seen from the Sun at the Summer Solstice, June 32 (noon at London), .;■-■■■ ., ■ -, --- r - '\ '---^ .'- '■ - • ^■' - .\* --■ .- -^Jt-^: '.^*--~*-- • . "•'^■■r,^ ^>r#«:' represent summer, for you will see from what has been said before, that if the north pole be turned away from the lamp, the nights are longer than the days;- when it is upright they are equal; and when it is turned towards the lamp, the days are longgy 3P SCIENCE PRIMERS, [§IX. i# than the nights; but the earth's axis does not alter in its direction, as we always find that the axis points very nearly to the same star, called the pole-star, at all times of the year. , .,4,. ,„.,,» . .,, ^.,u ^ 80. We must therefore try another method. Move ' » n »»* t>«. *•> •> A»-t. <*^-ft-v *vr'« fvvrf .'CiwtAsJAi'xW. 4« • ivw^- '^fi' iflw^iy*^*!**^ ■ § XI.— WHY THE MOVEMENTS OF THE SUN ^**'* AND STARS APPEAR DIFFERENT IN .^ DIFFERENT PARTS OP THE EARTH. ^^89. I must now endeavour to explain how it is that, as seen from different parts of the earth, the motions of the heavenly bodies appear to be very different. 90. Not only at the poles is there a day and a night, of six months, and not only at the equator are the days and nights always equal, but at the poles the stars seem to travel round a point overhead, while at the equator the stars which travel overhead seem to rise and set almost vertically, and not on a slant as they da in England, America, and Australia. < 91. We have already become acquainted with risings and iiettings as seen here, but let us observe the stars, not east and west, but in other parts of the sky, and see how they move ; you will see that in England the stars near the south rise only a little east of the south, get to the highest point above the horizon exactly south, and set as far west of south as they rose east of it. Those that we at first see rising in the east, pass over the south much higha- above the horizon, and set in the west again. The stars near the north neither rise nor set, never going below the horizon, but moving in circles round a point in the heavens, marked by a star called the pole star, a star easily found by its being pointed at by the pointers of the Great Bear, as shown in the diagram (Fig. 21). 92. Now, to illustrate this, take a small globe, make its axis upright, and in order to indicate the horizon Da 36 SCIENCE PRIMERS, [8X1. of any place quite plainly, cut a piece of card about the size of a penny and gum the centre of it oa,^e UP pen CULMINATION W POLC STAH 10 il LnWFH niLMINATION I ■■t\ Fig. ai. — The Pole Star and the Constellation of the Great Bear, in four different positions, after intervals of six hours, showing; how the Great Bear appears to travel round the I'o.u Ltar. ->i-**^' *w«i *j>^-^ iA^ - globe as near the upper axis or north pole as the mounting will permit, or put it on the axis if you can ; then a person standing at or near the pole would be able to see everything above the card, but not below — in fact, the edge of the card represents the horizon. Ndw spin the globe to represent the motion of the earth, and watch what the* appearance of the stars re- presented by the pictures on the walls (Art. 53) would be to a person standing at the pole. You will at once see that the card simply turns round like a wheel, and the pictures that were above it at first remain so. So the stars would not rise or set to p, person at the pole, ASTRONOMY. 37 but remain at the same height above the horizon, and only apparently move round the points of the com- pass ; the pole star being of course overhead, and the stars turning in circles round it. If you fix on a picture on the walls below the plane (Art. 67) of the piece of paper to represent the sun, you will see you cannot make it appear to rise or set by turning the globe round, it can only be thrown above the horizon by tipping down the globe as is done to represent the seasons. Now you will recollect that for one half of the year the north pole of the earth is tipped towards the sun, and during the other half away from the sun, so that it can only have day during the summer half of the year, and night during all the winter ; and if you will look at Fig. 20 you will see that during the summer the whole of t- . small circle round the pole is lighted, so that there is no night there as the earth turns round, and in winter foi the same reason there is no day, but in spring and autumn half the circle is light and half dark, so that every place is brought by the turning of the earth into daylight and back into night every twenty-four hours. 93. So much then for the view of the heavens at the pole. Now let us examine what takes place at the equator. To do this, gum the disc of card on the equator, and turn the globe. You will see that it no longer turns like a wheel, but turns somewhat as a penny does when spun on its edge; and on turning the globe half-way round, aq entirely new set of stars appears above the horizon, represented by the edge of the card, the two places in the heavens pointed to by the poles of the globe will be just on the horizon, tihe north pole-star just on the northern 38 SCIENCE PRIMERS, [§Xi. 11 ilS ■If,' !! \\ m III > part of the horizon, and the south pole just on the southern part of the horizon, and the stars which rise due east will pass exactly over the paper, and set due west as the globe is turned. ,l j^^i 94. If you fix on one picture to represent the sun, you will see that the globe can be just turned half- way round while the sun, or the picture representing it, is above the paper horizon, and half-way round while it is below it ; and as the earth turns round once every twenty-four hours, the sun will be twelve hours above and twelve below the horizon, so the day and night at the equator are always of equal length, and by tipping the globe to represent the changes of seasons you will find that the length of a.. day Qi night remains unaltered. ■ *y:^ 95. Now try for yourself, and place the card in other positions on the globe, beginning at the equator and going up to the north pole, and watch the gradual .change in the apparent movements of the stars in rising and setting. ,^^,,.,,,.^;^^.^.j nh^m&rm''humm^ 96. All that has been said refers to the apparent motions of the stars as seen on the equator, or to the north of it; so, in order to examine' the apparent motions of the stars visible in the southern hemisphere, you must stick the card at different places south ot the equato'- f^f the globe, and turn the globe and observe what takes place. First place it between the equator and south pole, to represent the posi- tion of an observer in Australia, then the equator will be north of him instead of south, and his pole south instead of north, as in our hemisphere, and if he looks towards the north he will see exactly the ^ame rising and setting of *he stars as he would ?ii the ASTRONOMY, 39 nottnerri hemisphere ; but nis nght hand will be towards the east and his left towards the west, so that the stars will rise on his right hand and set on his left, traversing the heavens in an exactly opposite direction to that they take in the northern hemi- sphere. Kurther, he will see near the northern horizon the stars seen in England near the southern horizon, the northern stars being altogether invisible to him. 97. In order to make the apparent movements of the stars visible in the southern hemisphere more plain, call the upper pole of the globe south, and the lower north, and turn the globe contrary to the way in which you turned it before ; for the earth appears to revolve in a different direction according to the position from which it is viewed, like the hands of a watch, for they go in one direction if looked at on the face, and in the contrary direction if looked at on the back, supposing the watch to be transparent; so to an observer in the southern hemisphere the earth appears to rotate in the opposite direction to that as seen from tlje northern hemisphere, and conse- quently, if we make the south pole the uppermost we must reverse all the motions including its motion round the sun. .-v...>..H.a. ■^^.j.^^i,^^^, 98. When you have done this, bring the true south pole of the globe to the top, and then experiment with the paper horizon as before. ■^''^'^W" 99. On the globe you will probably find a " wooden horizon," this represents the horizon of the centre of the earth, as we have supposed the circumference of the card disc to represent the horizon of a place. Ssta 40 SCIENCE PRIMERS. C§I. Hi 1 ( I ^jd mm. n o ?^. n.-^THE MOON AND ITS MOTIONS. ^^ Z^C,^ t IX— THE MOON TRAVELS AMONG THE ^^^ .. I . '.^^^y)-'\.' STARS *"' -''■' ^^^^■f^^^w.ii^m 'iV,i^^ 103. It is now the moon's turn. Look at it some fine evening, and notice its position amongst the neighbouring stars; it is difficult to see small stars near it, so it is best to take an opportunity when it is near a large one. Observe it again some hours after- wards, or, if need be, on the following evening ; you will at once see that it no longer occupies the same position among the stars, but that it has moved among them •1^3 .01.JI ASTRONOMY, 4« considerably towards the east. It will be observed to rise later and later every day, by three quarters of - an hour to an hour, as is easily noticed by timing its rising for a few successive days. It keeps on losing, as it were, on the sun, till, from being seen at sunset, it does not rise till just before the sun in the morning After this, the sun apparently passes it, and a few evenings afterwards it is again seen in the west just after sunset, only to lose on the sun and be over- taken again every twenty-eight days as before, in the same manner as the hour-hand of a clock is overtaken and passed by the minute-hand, ^k, -r^p^^i^W --'■- «iivio4. We have now made our observations : let us see how they can be explained. We must return to ^our orange and lamp, and, in addition, shall require *% much smaller orange to represent the moon. Now )rkeep the orange, representing the earth, still, and *move the small one representing the moon in a circle %ound it, as the earth moves round the sun. ^ 105. We have to see if th.^i motion will account for our observations. *. F"vst, let the moon be at E -(Fig. 22), in a line witii he sun, and as in such a *^position it would clearly appear to us to be a the sky near the sun, then it will appe^ to rise and set at the same time as the sun does, and on twisting the earth round on its knitting-needle, this »vill at once be clear. Next move the moon co T to re- present its position a few days later; you will now see that the sun will set some time before t- j moon, for to a person at A the sun is just ., but the "moon is above the horizon. Again, move the moon to F^ and you will see it is just south of the »observer at Ay when the sun has set, so that it has lost about # SCIENCE PRIMERS. [§n. .1: ;■; :i six hours on the sun. Move it further on fo' Cf alid it will just be rising when the sun is setting, and will ^ be south at midnight, having lost twelve hours on the sun, as will be seen supposing an observer to be at D; move the moon further to H^ then to the observer at A^ to whom the sun has just set, the moon will not have risen ; having lost eighteen hours on the sun, it will rise at mid-night, as will be seen by the observer at D, To the observer at C, the moon is southing and the sun is rising ; move it on farther to K^ it will nearly have lost a whole revolution on the sun, and will rise about twenty-one hours after it, if we reckon from the time they both rose together (or three hours be- fore it, if we reckon the other way), and in two or - MAI three more days they will both rise together again. Now it is clear from what we have seen that its losing \ on the sun may be accounted for by supposing it to travel round the earth in about twenty-eight days. And this we know to be the case. t. i>»i § II.— THE MOON CHANGES HER FORM. ■■■'.y^r-^i-^ffM^'.^-'>\'- • .!- ■•■"■'.•:.- '■ 1.' ■■ :'■■-■■,■- ^ ■.. ■■' ■ ■-■■' '•■.; ■ ■ '■'{::,■■•■■'•■■" .,■'■■ ^'^'. . :,-,-. .. 1 06. We have thus explained the moon's own motion among the stars, but something else happens to her: as she moves round us, she changes her form from a crescent to a circle. These changes have become so familiar to us, having heard of the changes of the moon as far back as we can remember, that we are apt to look on them as a matter of course, without inquiring into their cause. Let us ask the question, " Does the moon really change ?" No, it is always there, but a portion is sometimes unillumi- nated and invisible to us. ■Q I. :~ fi ASTRONOMY, 43 T07. Observe the moon some evening ; suppose you see it at the "full moon" as it is called, when it appears round, like the. sun : observe whereabouts it is in the sky, and you will find that it is on the opposite side of the earth to the sun, and that it consequently rises at sunset and sets at sunrise, in fact it is in position G (Fig. 22) ; now place the ball representing the moon at G on the opposite side of the orange to the sun, then the half of the ball, which is white in the diagram, ?\ ^^..L,;d-(|qn? i^/U'tO' 3 -:•>!. C o M a Dhoiti 'i!^;//. i>op '--"". ^ - ilG. sa.— The Moon's motion round the Earth, g rijll M* - *? £i',,F'.J., x~ will be mummated by the sun, and the other half, op- posite to it, will, of course, be dark, in the same manner as we have night when the sun is shining on the other side of the earth to us, and if you place your eye near the orange, you will see all the bright portion and none of the dark side ; it is then full moon, and this appearance is represented by the white circle M, So that it is now clear that at full moon the moon is 44 SCIENCE PRIMERS. C§n. lit ;'. i on the opposite side of the earth to the sun, and we see therefore the bright side.>r* vj i/w« ^muc.. .. a 1 08. After the full, the moon riseis, as we have seen before, later and later after sunset, and we will suppose you observe it a week after the " full." It will rise, as you will find, about midnight. Rather late, you say, to sit up, but the day of astronomers is other people's night. The moon now is no longer apparently round, only half of it is visible. Return to the diagram : in what position is the moon if it rises at midnight ? It is midnight to an observer at D, and the moon to be rising must be at If» Place the ball, therefore, at Iff and the eye at £>; now the part, white in the diagram, is the bright half illuminated by the sun ; but in this position the whole of it is not visible, but only half of it and half of the dark portion, you will there- fore see that we ought to have the appearance of half moon, N, in this case, which we do in reality. ,i *, 109. Let us continue our observations. If it is too late to sit up after midnight, try and get up before sunrise and you will see that, as the moon is appa- rently overtaken by the sun, it will get more and more crescent shaped, and when at JC it appears as at O, till it is lost in the sun's rays and comes to position £. How ought it to appear now ? Place the ball between the eye and the lamp, and you will see the whole of the dark half and none of the bright portion. It is " new moon ; " look at it a few days after, when it will be visible just after sunset. It will appear in a thin crescent, and will be in the position marked T in the diagram. Place the ball in this position, and by placing your eye close to the orange you will see just a crescent of the bright half, and a large portion of the dark half. '■*^r .«Jtl ajA:ASTRONOMY, m. 4S 1 10. As the moon appears to get further and further from the sun, and to set later and later, more and more of the bright half will be seen, till we get to half moon in position F. It is now south at sunset. Place the ball in this position, and your eye close to the orange, and you will see the observation is ac- counted for. Another week more and the moon again becomes full, and opposite the sun.'tvu'UA ^ .* * ^jugiix tj III. All these observations may be thoroughly mastered by standing at a distance from the lamp, or gas-light, which should be the only one in the room, and moving an orange, or ball, round your head, when all the changes of the moon will be rendered clear to you. The moon, therefore, revolves round the earth in the same manner as the earth goes round the sun, passing from full moon to full moon in about twenty-nine and a half days. , , , ^^1 III.— HOW THE MOON CAUSES ECLIPSES. 5si 112. From what we have seen, you might think that the moon ought to pass between us and the sun every month, and produce what is called a total eclipse of the sun ; but, for reasons of which we shall presently speak, it sometimes passes a little above the sun, and at others a little below, when there is no eclipse at all, or it passes over a part only of the sun, and so only covers a portion of the sun's disc from our view, producing what is called a partial eclipse. 113. Let us see if we 'jan make matters clear with the use of our orange and ball i V m SCIENCE PRIMERS. [% in. 11)5 \\ 114. Set the lamp on the table, and stick the knitting needle supporting the orange into a large pincushion at some distance from it; then take the small ball representing the moon and suspend it by a string, so that you can move it round the earth (Fig. 23), without the fingers casting a shadow on it. Now bring the moon between the sun and earth, holding it near the earth as at C (Fig. 23), so that the shacfow of the moon falls on the earth: wherever this shadow falls on the earth there will the sun be invisible, and there will be a total eclipse at that place. At other places on the earth, as at B, which the darkest part of the shadow ■'■' '' -• v\: 1 % ... i . ( ^ ^ Fig. 23. — ^Total Eclipse of the Sun. !.„ fj-'tfj^ju jT" i It-'. / liHt tt 47 115 Now move the moon further away from the earth, to say D (Fig. 24), and you will see that the shadow of the moon is not sufficiently long to reach the earth, so there can be no total eclipse, the moon being so far away that its disc is not sufficiently large to cover the sun completely, so there remains the outside edge of the sun visible j this sort of eclipse is called an annular eclipse. .vsii !utr ) 3/*^^^ 116. All this will be clearer if the orange be re- moved and the eye placed in its stead. First place i^Ela ;:>|-\Mj j^^M h ii m>4u-%'( miy^^-^i ■ ?^^^ ^i .^i^i'hp IMffyf'iM ^-Tii f-' ■.v'^.i. Mi i^::i -S ^i^. k'' ri'- i^iG. 24. — ^Annular Eclipse oi the buu. your eye where the shadow was (Fig. 24), that is, in the umbra of the moon, and you will see a total eclipse. Then move the eye a Httle lower, still keeping the moon in the same place, and you will see a crescent of the sun, in fact a partial eclipse, and the furt' eryou move your eye from it, the more of the sun you will be able to see. Now place the eye at A and so see a total eclipse, and move the moon gradually away from you, and you will see the moon apparently 'in m.,yy t ) ssaz 48 SCIENCE PRIMERS. [§ ni. ft » I getting smaller, so that at D (Fig. 24), it is no longer large enough to cover the sun, and you see the bright edge of the sun round the moon ; in fact, an annular eclipse. 117. Besides eclipses of the sun, there are eclipses of the moon, occasioned by the moon passing through the shadow of the earth. You will readily understand how these happen by placing the lamp and orange as before : on passing the ball, repre- senting the moon, round on the opposite side of the earth to the sun, it will go into and throtigh the shadow of the earth, and will be darkened, not, as ejilBaJW^ is in^M%.-%^^ of the moA'S^^: «^'^^^^^?.^4t in the case of an eclipse of the sun, %f Im opaque body coming between us and the sun, but by its being shaded by our earth (Fig. 25). ^ 118. To an observer on the moon during a total eclipse of the sun, the earth would appear to have a black spot on it, moving rapidly across it; and surrounding the spot would be a circle of half shade, the penumbra, in which a partial eclipse is seen from the earth ; but in the case of a total eclipse of the moon, the shadow of the earth entirely envelopes the moon. iiQ. You will have understood by this time that an ■'V; ASTRONOMY. 49 an eclipse of the sun can only take place at new moon, and an eclipse of the moon can only take place at full moon. The reason being thai when the moon is between us and the sun, that is, when an eclipse of the siin can happen, the moon's dark side will necessarily be turned towr ^-ds us ; and when the moon is on the oiher side — on the opposite side of us to the sun, that is, when an eclipse of the moon can happen, it must have its bright side towards us. . 120. We have spoken (Art. 112) of the moon passing sometimes above, and at other times below the line joining the earth and sun, and, as you will see by referring to the orange and ball, an eclipse of the sun and another of the moon must happen every month if the moon did not so pass. 121, Let us see how we can account for the fact that the moon does thus pass sometimes above and sometimes below the sun, thus preventing monthly eclipses. We have found that the moon revolves round the earth in nearly a circle (with the earth at the centre) called its orbit or path. Let us represent this orbit by a piece of wire, bent in a circle round the orange, and let the moon be represented by a large bead or a small ball strung on it. Hold the ring of wire so that the earth (orange) is in the centre, and move the moon on the wire round it, and you will find that if the ring is held horizontally the moon will pass between the earth and sun, represented as usual by the lamp, at every revolution. Now this we have observed is not the case with the real moon, and in order to make the bead pass above or below, the part of the ring between the lamp and the orange must be tipped up or down. 122. To make this clearer, get a tub of water as s so SCIENCE PRIMERS. [§ "I. 14 'X': before, and float in the middle a ball to represent the? sun, so that half is above water and half below. Float another small ball near the side of the tub to repre- sent the earth, then ihe earth can be floated round the sun, to represent its annual path. Now, as its orbit will lie on the surface of the water, this surface, as we have seen before (Art. 67), represents the plane of the ecliptic. 123. But we have already suspected that the moon's orbit is inclined to this plane, so that at certain times no eclipse takes place ; and if we take the II A 'iMSt i£^l;imfi S^as^l^ ,^^^ ^^¥* i^^mit^ rsv Fi& 26.— Shewing the inclination of the Moon's orbit to the plane of the f wire ring as before, to represent the moon's orbit, and ^^ place it round the earth, dipping one half of the ring below the surface of the water, and keeping the other above, as represented in Fig. 26, where the full line i'* Tfv ai - ASTRONOMY. '"Wt. 51 le at e- id Its he ' the': at ' the'^ :>;^ Oil ba«ti| of the f i ring other i UUne indicates the part above water and the dotted line the part below, we represent the inclination 01 the moon's orbit to the plane of the ecliptic, and the line joining the points where the orbit cuts this plane is called the line of nodes, and B asid D are the nodes. 124. This will render it clear that eclipses, suppos- ing the orbit of the moon to be inclined to the plane of the ecliptic, could only happen when the moon is at the part of its orbit near a node when she comes in a line with the earth and sun, for only then does she in her revolution pass between the sun and the earth. At the other parts of the orbit there can be no eclipse, because the bead on the ring would at its nearest approach to an eclipse be below or above the water, and not on its surface in a line with sun and earth. And as eclipses do not happen every month we know that the moon's orbit is inclined as we have supposed it to be. 125. We have seen before that the plane of the earth's motion round its axis is inclined to the plane of the ecliptic, and we now find that the plane of the moon's motion round the earth is inclined to the same plane. We' should now endeavour to understand how the amount of inclination is fixed in each case. 126. To do this astronomers divide all circles, whe- ther large or small, into 360 degrees (written 360°), (see Fig. 27), and if we draw two lines firom the centre of a circle to the circumference the number of degrees intercepted between the points where they cut the circumference is the measure of the angle between the two lines^at the centre. Now 360 is four times 90, sd that two lines containing a quarter of a circle make an angle of 90° between them. You will see K a y^' r;C #--.-» •^ M' ftS* SCIENCE PRIMERS. 'V [§IIL that the size of the circle is of no consequence, for if you draw a number of circles, one inside the other, all having the same point for their centre, and from the centre .draw two lines intercepting a quarter or 90° of the outer circle, then you will see that it inter- cepts also a quarter of each of the others. Each 90® is called a right angle, and two lines which make an » t ^^ -**...! ****• ^7* — Division - 134. Astronomers have found out the weight of the earth, and of the moon, and they also know how many cubic miles (or cubic inches) each contains. They can therefore easily find whether a cubic inch or mile of the materials of which the moon is built up weighs less or more than a cubic inch or mile of the materials of which the earth is built up; in other words, whether the earth is less or more dense than the moon. And they have found that a cubic inch of the earth's materials weighs ij times as much as a similar quantity of the moon's materials, hence they say that the moon is only | as dense as the earth. .. 135. More commonly the weight or density of a cubic inch of water is taken as i, then we say that the density of the earth is 5 J, and that of the moon 3^ times greater than that of water. Thus then we have in the case of each celestial body : '^ ^^ *^ a. Its volume expn >sed in cubic miles or cubic inches determined firom iw diameter, .. -^ „ .^^i V b. Its weight or mass, that is torsi^K6w raaiiy tons it weighs, this is determined from its action on other bodies.^.^^ I ^* ai^^*;^^ ri c. Its density, that is how much a cubic inch or cubic mile weighs ; this is found by dividing its mass or weight by its volume. ??^^ % -. 'J; . "> i ' n !H \i '^ SCIENCE PRIMERS. 136. The same side of the moon is always turned towards us, for as the moon goes round the earth it^ slowly turns on its own axis, and makes one revolution^ in exactly the same time as it takes it to get rounds us, just in the same way as you would do if you were to take hold of a pole stuck in the ground, with your - hands, and go round it, always keeping your face turned towards the pole. You would then see, by looking at adjacent objects, that you turned round once every time you went round the pole, and you will probably become giddy, thereby giving conclusive evidence of your rotation. , - . 137. It follows from this fact that tKe mooti olily turns round once on its own axis during each re- volution round the earth, and that the lunar days are about 29 of our days. We are lighted by the sun for about 12 hours, or ihe half of 24 hours ; each portion of the moon is lighted for about 14 days, or the half of 29 days, so you can imagine how intensely heated the surface must become during the lunar day, and how cold the opposite side must get during the 14 days' nicht ''•* ■'^'^-*'^'^^*'^ *''^^ ''-}}^^..^- V^ i''j:Miiy'yxqoinoi,Hboq -THE sbLAIl SYSTEM. X~ttOW BODIES LIKE fHE EAR'TH, NfiA ^^M .''■*>'; K':^'- THE SUN, WOULD APPEAR TO US. ER; if 138. So far as we have gone the earth on which we dwell, the large sun and moon, and the tiny stars, are the only bodies with which we have dealt •V ' - V ^ I. fl"!' '.'A:. nil ASTRONOMY. 57 139. Let us see what we should observe in the heavens if there were other bodies, not shining by their own light — other earths like ours, revolving round the sun as we do. How would they appear to us ? And first let us take the case of a body travelling round the sun but at a less distance from him than we are. Let us think. Take the lamp to represent the sun, the orange for the earth, and the ball used for the moon to represent the other earth ; then all we have to do in order to represent the appearance of the new world in its journey round the sun, is to move the ball round the lamp, and see how it appears from the o^fi^nge in its ditfeti^t positions. I'irst place it wi the >fj'Otr|y(:..|:|jx-f^ i«wc- ilf^' i ; /;■«!, ^' *'hrife 151 Bm |.i: :i:.J? 4u 'jo\ p^ tk/^m q- Fig. d8. — Diagram lllustmting the mbtioiis and app^irances of a body between us and the sun. position represented by A, Fig. 28, between the lamp and the orange — then it will appear in the same line with the sun, and accompany the sun in its path across the sky, at which time of course it will be in- visible on account of the superior brightness of the sun, but it will set and rise with it ; now move it tc B — it will then appear on the right side of the sun, and will rise before daylight and set before the sun, so that it would only be seen before sunrise, changing its place, — " wandering '' among the stars from day to day (the word planet means a ** wanderer"), to be put out like the stars by the day. Move it to position C—it will then rise f 58 SCIENCE PRIMERS, [§n. and set with the sun, and will be lost in the sun's rays as at A, Again move it to D — it is then on the left side of the sun and will rise after daylight, and set after . sunset, so that it will be seen only in the evening. A ; little consideration will make it plain that this body will go through the same changes as the moon, and again that we can never see it at midnight. But there will be an important difference. As we go round the sun, keep- ing always about the same distance from the sun, the sun always seems to be about the same size ; and as the moon goes round the eiarth, keeping about the same distance from it, the moon always seems to be about the same size. Mind, I do not say the same form. But the new earth about which we are now think- ing goes round the sun; so it will sometimes be between us and the sun and sometimes on the opposite side of the sun, so that its distance from us will vary \ therefore, its apparent size will vary. 140. Hence, if we were to examine this new earth with a telescope, we should see it vary in size and also in shape like tiie moon, and if its atmosphere were clear, we should see its seas and continents^ and so by their motion we should be able to ascertain how fast it turned round on its axis — whether its day was longer or shorter than ours. ^^^ :-.^|^ t^^^ >o fc § II.—HOW BODIES LIKE THE EARTH, FURwf^ «fei THER OFF FROM THE SUN, WOULD APPEAR TO US. .»..^A_-,i4 -»»1»i»%^ a 141. In order to represent the appearance of an earth outside us, we have only to move the ball in a circle round the sun, outside the earth's orbit. Let 1 " ^- ^ 4 '^ ASTRONOMY. ii ^MWo***'^-^ V 59 us begin by holding the ball on the opposite side of the sun to the earth — then it will be lost in the sun's rays, and on moving it further round in ♦;! e contrary direction to the hands of a clock, it will be seen on the left side of the sun, and will therefore set after it just as the interior earth did ; but as you move it on after it has made a quarter of a revolution, it appears to recede further and further from the sun, Ji s^^ >^d oi afiUK-^i^.-'-j £% -5^ Ixliibfie Gv^ "{/. iDsU*, *J0''fc> *J£*^ »'* Fig. sg.— Diagram aHustrating the motion of a body travelling round the sun outside the orbit of the earth. instead of again approaching it, and passing between the earth and sun; and eventually it comes to the opposite side of the earth to the sun and rises at sunset, and is visible in the south at midnight, which as we have seen was impossible in the case of a body between the sun and the earth. 142. You will also notice that nearly all the bright side is visible to the earth, although at the two positions corresponding to A and B, Fig. 29, it will 60 SCIENCE PRIMERS, [§ HI. show a portion of its dark side, so that an exterior earth would not go through all the changes that an interior oii» would do. While, therefore, the interior earth would appear to swing from side to side of the sun, unly the exterior one would take a sweep round outside our earth. Such a body will vary its size^ but not to so great an extent as an interior one. ?-t 8 Hi.— ARE THERE SUCH BODIES?— THE PLANETS. 143. There are such bodies as we have just been considering, both interior ones and exterior ones, and they are all called Planets, and the earth is called a planet simply because it, like them, would appear to wander among the stars to astronomers on the other planets, if such there be. The principal planets are eight in number, including our earth. They have been named after the ancient deities ; the two interior ones. Mercury and Venus, and the exterior ones. Mars, Jupiter, Saturn, Uranus, and Neptune ; the three first being smaller than our earth, and the remainder a great deal larger. 144. Mercury and Venus are known to be interior planets, that is, planets between us and the sun, because they appear to swing, as we have found such bodies should do, on either side of the sun. Mercury very seldom leaves the sun sufficiently to rise so early before the sun, or set so late after him, as to be visible. Venus, however, gets so far away as to be seen long after sunset or before sunrise, and is called the Evening or Morning star, accordingly. 145. The exterior planets, as we found such bodies [§ in. .n exterior es that an he interior to side of e a sweep ill vary its moT one. .4i^vS2^ y^,.:.^ ,„fl»^..u —THE ■;« ^ just been irior ones, le earth is em, would nomers on ; principal our earth, eities; the he exterior Neptune ; li, and the ,1 .i h l;|i>*" ^li' 3e interior the sun, ound such Mercury se so early , as to be / as to be [ is called iich bodies ■HMh : .I'v' ?f' ■» ./!»>. 1 J -J • '\\(tr\ , ''■-'%K Si^'-J-XSj^a^ .W-i- IWI-'-'. >/»■ ac o !>rfr^ Tfi^tf:: rr ■ "f",nrr»''^- >iool n i"' .■;»?>»■■■» .t U.U V-'' T'5»?9JII *>„ >V 'j'%- ■^^ tj-rt'^ ASTRONOMY, 6l should do, make a complete tour of the heavens. All these movements are, however, rather more com- plicated than we ha , e found with the orange and ball, for the earth is not fixed, but going roimd the sun quicker than the exterior, and slower than the interior planets; and, in order to represent the true apparent motions you must move the orange round the sun at a rate depending upon which planet you wish to re- present by the ball 146. The sun and planets revolving round him form what is called the solar system ; in fact, everything over which the sun has continued in- fluence is a member of this system. 147. Thus besides the planets there are other members of the system, namely, comets and falling stars, which will be mentioned again more fully here- after : all these bodies form a sort of family having the sun for their head, and on Plate II. will be seen a view of this system as it would appear when looked at from above; but it is impossible thus to give an idea of the true scale of the system. In order to do this, take a globe a little over two feet in dia- meter to represent the sun : Mercury would now be proportionately represented by a grain of mustard-seed, revolving in a circle 164 feet in diameter; Venus a pea, in a circle of 284 feet in diameter; the earth also a pea, at a distance of 430 feet; Mars, a rather large pin's head, in a circle of 654 feet; the smaller planets by grains of sand, in orbits of from 1,000 to 1,200 feet; Jupiter, a moderate sized orange, in a circle nearly half a mile across ; Saturn, a small orange, in a circle of four-fifths of a mile ; Uranus, a full-sized cherry, or small plum, upon the circum- • • ^'1 62 SCIENCE PRIMERS, [§ IV. ference of a circle more than a mile and a half; and Neptune, a good-sized plum, in a circle about two miles and a half in diameter. '^ *' 148. I have already told you that the earth's distance from the sun, represented in Art. 147 by 430 feet, is really 91 millions of miles, I cannot give you any idea of this distance. I can only state that if a train going at the rate of thirty miles an hour were to leave the earth on the first of January, 1875, it would only reach the sun in the middle of the year 149. Beginning with this rough idea we will now consider the interior planets — those, namely, which are nearer the sun than the earth. '%i. Ti-y^, § IV.— THE INTERIOR PLANETS. , Mercury. 150. Mercury, the nearest planet to the sun, revolves round him at a distance of about 35 millions of miles j the earth's distance from the sun being 91 millions, it has a diame^:er about one-third of that of the earth. It can be seen at certain times just after sunset, and at others just before sunrise, as it never quits the neigh- bourhood of the sun. It is eighty-four days in travers- ing its orbit, so that its year is less than a quarter of ours. Its orbit is represented in Plate II., and, like the moon's, is slightly inclined to the plane of the ecliptic ; tLat is to say, if the earth's orbit is supposed to be floating on the surface of water, part of Mercury's orbit would be slightly below the surface and part over. From the diagram you will see that Mercury ''% ASTRONOMY. 63 [§iv. '; and it two earth's 47 by "t give te that ir were 875, it e year ill now which evolves ^ miles ; aiilions, le earth. , and at I neigh- travers- larter of ind, like e of the pposed ercur/s ,nd part Mercury . will always appear to us near the sun. When it is on our left of the sun it apparently follows the sun on its daily course, and sets just after it ; when on the other side it precedes the sun, and therefore sets before it, and so is only seen in the morning, When it rises just before the sun. 151. If Mercury be watched with a telescope it is found to go through the same changes as our moon, and for the same reason. You will understand this from Fig. 28, where the ball may betaken to represent Mercury in its different positions as it revolves in its orbit. When it is between us and the sun (or in what is called inferior conjunction) we do not see it as its dark side is turned towards us, and as it moves round we see more and more of the bright side, till when it is opposite to us, or in what is called superior conjunction, we see the whole of the bright side. 152. Little is known of Mercury itself; we know not whether it has a land and water surface like the earth or is waterless like the moon, whether it is enveloped in a dense cloudy atmosphere which pro- tects the inhabitants, if such there be, from the intense heat of the sun, or not. We only know that its density (Art. 133) is greater than that of the earth. -Venus. 153. Next to Mercury comes Venus, at about 66 millions of miles from the sun, with a diameter nearly as large as the earth. It can generally be seen either just after sunset or before sunrise, according to its position in its orbit round the sim, in the same manner as Mercury, only its orbit being outside that of Mercury -jibiHB&bAalBi UJteJUW'^iitfrtlftti [iirtflAaaMMMfei 64 SCIENCE PRIMERS. [§iv. V . m%\ i;^ I '. m I it can get further away from the sun's apparent place among the stars, consequently we can examine it better. It is the brightest of the planets, and when visible )annot be mistaken. It takes 224 days to perform its annual revolution, and 23 hours and a quarter for its rotation on its axis, which determines the length of its day. 154. We have shown in speaking of the earth that the inclination of its axis produces the seasons, and that the pole of the earth, instead of being upright or perpendicular to the ecliptic, is inclined 23° (Art. 71). In the case of Venus there is affirmed to be an inclination of 50°, or about half-way between upright and horizontal ; the consequence is that the seasons there change to a much greater extent than ours do. 154. Venus also goes through the same change of phases as Mer- cury does, and of course for the same reason. Very little is known of the surface of Venus : certain dark n^arkings, however, are seen frequently with first- FlG. 30.— Venus, bhowing the markings on its surface. 'l- ■9 •I [§iv. ASTRONOMY, «5 t place better, visible arm its for its igth of th that IS, and right or Lrt. 71). . :ase of lere is be an iof5o°, lalf-way upright izontal ; gquence seasons a,nge to greater an ours :nus also mgh the mge of as Meir- 2s, and •se for reason. ; certain dth first- f ■'I'k rate instruments on the surface, which may possibly be breaks in clouds, through which the planet itself is seen. The density of Venus is about the same as that of the Earth. 155. If you will think a little you will see that in the case of Venus the apparent size as seen from the earth should greatly change, as the nearer she is to us the larger would she be if we could see her completely; so that, although like the moon she has phases, unlike the moon her size will alter. Let us inquire into this a little closer. When Venus is nearly between us and the sun — when, therefore, we can only see a fine crescent — she will be but some 25 millions of miles away from us (because we are 91 and she dd millions of Fig. 3i.-Apparent size of Venus, at its least, mean, and greatest distance from the Earth. miles from the sun> ; but when she is on the other side of the sun she will be 157 millions away from us i T9 U • ! ii ! I S I ! 66 SCIENCE PEIMEXSi •^ (that is, 9T millions firom us tc ne sin axd 6i from the sun to Venus on rhe ctiier ade . 90 size will vary in the proportion tf 157 no 25, to i; so that the crescent of Veacs^ wiii 21 part of a circle 6 times larger tiszn tnai presentKi Venus when she is full to as. These doemges .are shown in Fig. 31. 156. Venus and Mercniy, at times imat they ars on the earth's side of tiie sun, are vaSfe as black spots on the sun's disc. This is called s transit of Mercury or Venus ; that is, the passage of tie planet exactly between us and the son, so tiat it h seen on the sun's disc. 157. A transit of an interior planet. Eke an edipse of the sun by the moon, can only happen when the planet passes the sun at the time it is near one of its nodes, that is when it passes from one side of the plane of the ecliptic to the other. A transit, in other words, car only happen on the coincidence of the earth and planet both being in a line with each other at either node. A transit of Venus happens in 1874, and again in 1882, and not again for 1055 years. fiu'a'i' 158. Next to Venus comes the Earth, the planet on which we dwell, and which has already been described. We therefore pass on to the exterior planets. «-»m i m ^ <-.\^ib '\^^ .»i ■'■)?" -^dPu § v.— THE EXTERIOR PLANETS. - 159. The next membtst of our system is Mars. Mars revolves in an orbit having a mean or average distance of 139 millions of miles from the sun. It tt. ■niif ley ; black isit c^ of tie at it s edipse len the one of J of the n other of the :h other n 1874, rs. ; planet iy been exterior ICTC) mQ£' is Mars. average sun. It f ASTRONOMY. 67 revolves on its own axis in 24 hours and a half, making its days half an hour longer than ours. Its diameter is about one half that of our earth. 160. Mars requires 686 days to complete its annual revolution round the sun, making its year nearly iouble the length of ours. Since its orbit lies outside this planet never can pass between us and the sun, consequently it does not show the same phases as lus or Mercury ; it however at two positions in its crbit becomes what is called gibbous, losing appa- reatly its brightness to a small extent on one side, as «il be seen in Fig. 29, where the two positions, n^n the earth is at B, are marked A and B^ and ai these two points a small part of the dark side will be turned towards us, presenting an appearance like the moon two or three days before or after full. 161. When Mars is on the opposite side of us to the sun at M, it is said to be in opposition ; it is then at its nearest pomt to us (its distance being 139 — 91 = 48 millions of miles) and fully illuminated ; so then this is the time to examine the p.anet. Its orbit is, however, v^ory eccentric or oval, consequently it is much nearer the earth's orbit in one direction than in others ; and w^<« an opposition happens, as is the case when Mars and the Earth are in this position %y[ their orbits closest together, we have a most favour- able opposition, at which time Mars is only about half the distance ^ is from us at the most unfavourable one. The inclination ot its axis is nearly the same as that m t^ earth, being about 29°, m diat the Martial seasons must be vmy simiiar to ornt^ ifiih Whea looked at with the eyt alo^e, llfem of a reddish tot,^ by whicfc k ssm hm m 9 2 mmmi '\ > 68 SCIENCE PRIMERS. I J: ■ i 51 1 1 ' 3 [§V. recognized, but when seen through a telescope the redness in a measure disappears, and the planet appears to have a bright surface, on which are darker portions, the former being the lands, and the latter the seas. Mars is the most remarkable among the planets in this, that it appears to us as the earth would appear to its inhabitants. Around the poles the surface appears white, and on watching the spots Fig. 32.— Mars, showing snow cap at the pole, and the lands and seas. from time to time each is seen to grow small as summer is approached in that hemisphere while the opposite one gets larger m winter, so we suppose these to be the polar snows corresponding to those on our earth. The drawing will give sorae idea of the appearance of Mars as seen in a large telescope, r .r. [§v. le the planet darker latter ag the earth 1 poles 2 spots ASTRONOMY, 69 md seas. small as vhile the suppose to those \ idea of ;elescope, one of the main features being that instead of there being about four times more water than land as on our earth, there is on Mars about four times more land than water. The Asteroids. 163. Beyond Mars we come to the Asteroids, or minor planets, a number of small bodies not varying Fig. 33.— Mars. View of another part of the planet. greatly in distance from the sun, and revolving in orbits outside that of Mars. Vesta, Juno, Ceres, and Pallas are the principal ones, but they are only some few hundred miles in diameter, and are barely visible to the naked eye, if at all, and from their smallness are worth little notice. Their orbits are more inclined to ■fe II \i\ \\ m ; 70 SCIENCE PRIMERS, [§v. the plane of the ecliptic than those of the larger planets, but we have no knowledge of the inclination of the poles of these small planets to their orbits. Their number is large, about 130 ; and we say about, for several are discovered every year, and the names of nearly all the deities must have been used for them. The greater number of these are only equal to a loth magnitude star in brilliancy, and their surface may possibly be not much larger than the area of a good Scotch estate. Jupiter. "-.v- 164. Outside the orbits of the numerous asteroids is the largest planet of our system, Jupiter, a body that has no doubt been pointed out to you some time or other. When above the horizon, it is unmistakable by its excessive brightness, being only surpassed by Venus, which can generally be recognized from it by its proximity to the sun. Jupiter revolves in an orbit at a distance of 476 millions of miles from the sun, com- pleting his year in 4,333 days. 165. When observed with a telescope of moderate power, Jupiter appears of an oval shape, very much flattened at the poles, and crossed by several dark belts, as represented in the figure ; large black spots and other markings of which we shall say more presently, are also frequently seen on the surface, and from the motion of those markings, the time of rotation on its axis has been ascertained to be about 10 hours, that is less than half one of our days, and its dia- meter is found to be about ten times the diameter of our earth, so that the flattening of the poles and the m /!-/.'J:J.'>ii,-:9.jr-lJ.^I;iV,fi\-_.;. ASTRONOMY, It protuberance of the equator must necessarily greatly exceed that of our earth, for the velocity that the equator moves at must be twenty times the velocity of our planet at the equator, or 20,000 miles per hour. 166. We have mentioned the belts and other mark- ings on its surface; it is probable that Jupiter is covered with clouds, giving rise to its bright appearance, and that the dark belts are openings in the clouds through 1.: !i ,;:■!*:(; <- -. ■ Fig. 34.— Jupiter, showing the cloud belts. I'^'KKf i:;;UO which we see the darker surface of the plane^ oit more probably of lower beds of clouds beneath^! The number and size of the belts are continually changing, and bridges of cloud are constantly being thrown over the dark spaces, clearly showing that it is not the surface of the planet we see, but only a very cloudy atmosphere. ^ r v.:x -...,,/::■.... ;,,);.^y^l^ $ m B I . -.St. P > Vi f 72 SCIENCE PRIMERS. [§V, 167. So far as we have gone the planets have been unlike the earth in one respect, they have no moons. Jupiter, however, has four satellites or moons revolving round hin?> and going through the same changes as our own. They are all nearly of the same size, about 2,000 miles in diameter, but at different distances, and consequently they take very different times to revolve round their primary, Jupiter, the first taking less than 2 days, the second 3 J days, the third 7 Fig. 35. >- Diagram explaining the eclipses, occultations, and transits of .,,- , ..: ..,,. ^ 't Jupiter's satellites. days 3 fioiifs, tie' fourth i6| days. They all re- volve in orbits very slightly inclined to the plane of Jupiter's orbit, and consequently whenever they pass between the sun and Jupiter there is an eclipse of the sun visible on some part or other of the planet's surface j only the fourth has an orbit sufficiently inclined to enable it to pass above or below the line joining the sun and Jupiter, this prevents it from causing an eclipse at every revolution. For the same l§v. ASTRONOMY, 73 s ti reason of course the moons also are eclipsed at every revolution by the planet's shadow. 1 68. When viewed with a telescope the moons appear to oscillate on either side of Jupiter (just as the interior planets appear to us to oscillate on either side of the sun), and in their passage from one side to the other they generally pass over the disc of the planet; there is then what is called a ** transit" of the moon over the disc. We also see the shadow of the moon traversing the disc whenever we are so far from the line joining the sun and Jupiter, that the moon does not cover the shadow. The moons in passing round on the other side at times suddenly disappear, or are eclipsed, when they pass into the shadow of the planet, but we may be in such a position that Jupiter's shadow lies on the opposite side of the planet to that behind which the moon passes ; the satellite then goes behind the disc uneclipsed, and is said to be "occulted.'* The diagram will make this clearer; when the earth is at the point E of its orbit, the moon N appears in transit, while the M is occulted and O eclipsed, and from this point of view every satellite must be occulted before it is eclipsed ; but when the earth is at i^the moon J/ is no longer occulted, and will pass into the shadow and become eclipsed without an occultation, and from this point P will be in transit and O also eclipsed, but as soon as it leaves the shadow it will be behind the planet, and will reappear from an occultation. : , ; 169. The inclination of Jupiter's axis is very small, only a little over 4°, so that there can be no appreci- able change in the Jovian seasons. Although the size, or, more correctly speaking, the volume, of Jupiter is '->. IMAGE EVALUATION TEST TARGET (MT-3) ■^ ,.^4 <3 i I.I 1.0 S!i»- l!M ^ IM 12.2 14 2.0 III 1.8 1.25 ! == ! U 1.6 ^ */' ■^ V ^ pm Va >> ^<^^ ^. .^* W N> t^ (? / Photographic Sciences Corporation 2: WEST MAIN STREET WEnSVER.N.y. 14580 (716) 872-450'' I I '%'- 74 SCIENCE PRIMERS. C§v. more than 1,300 times that of the earth,^ — ^^that is, 1,360 globes of the size of our earth, if made into one world, would only be of the size of Jupiter, — still its weight is only 300 times the weight of the earth, so that the materials composing Jupiter are of a much lighter kind than those composing the earth \ thus representing the density of the earth by i, Jupiter's density is less than \, i^no0f)oiq siadq? (^bjb ^kqi^ 170. We i^ext come to Saturn, a truly grand sight itf a telescope, Saturn having, besides eight moons, an immense bright ring surrounding the globe. This Fig. 36.— Saturn and his rings. .,? .^J, ..a r^A-ft planet revolvesfn air oMtd^Lhmxtfi miHicins of miles ^ from the sun, taking 10,759 days, or nearly thirty of our years, to complete its year, and having a diameter nroe r§v. , 1,300 to one still its Tth, so much ; thus iipitefs mo wo iight M ►ns, an This ^« ASTRONOMyi:y>^ 75 1 times greater than that of the earth. From observa- tions of spots and belts on the surface (somewhat similar to those on Jupiter) the time of its diurnal revolution has been fixed at about 10 J hours, a little longer than that of Jupiter, and it is probable that Saturn has much the same constitution as that planet, as it appears to us to be covered with an extensive cloudy atmosphere producing belts as on Jupiter; it is also made up of very murh lighter materials than our earth is, materials of only half the density of those composing Jupiter. Saturn's axis is inclined at an angle of ab^mt «6i% SQ th^are are seasons there ason our earth.'- ^ -' ' ■- ..j-.'^:,," ^,;->-: ^-^ ^^-rrrt,'"^ Mfrn-rj^M \" 171. Now as to the rings, what are they ? Their general appearance is that of three rings lying outside each other in succession as shown in the diagram, Figr 36, the diameter of the outer ring being about 166,000 miles. The two outer ones are the brightest, the inner or crape ring being only just visible in a large telescope, the ball of the planet being seen through it In spite of their enormous breadth, die thickness of the rings is only about 138 miles, and when edgeways to us, as is the case in certain positions, when Saturn moves in its orbit, they are barely visible ia the best telescopes. It is thought that the rings represent a vast assemblage of small satellites or moons revolving round Saturn. 172. The moons of Saturn, eight in number, are not of such interest as those of Jupiter. Their distance from us precludes us generally from observing their eclipses and occultations ; their orbits alio are largely* ' inclined to the orbit of Saturn, and consequently eclipses are rare. 76 SCIENCE PRIMERS. [§V. .I'wvA 173, We next come to Uranus, of which little is known, its distance — 1,753 millions of miles from the sun, being so immense ; it takes 30,686 of our days to complete its annual revolution, and it is known to have four moons. Its diameter is four times greater than that of our earth, and its density is about \ that of the earth. -'>^49ail^'Y^'«*iJkeau 'Mm'-^^ •F)iX^"J^iBdtl ■ffv. ;,. NEPTlTiyE, lb kM'^" 'oa -^ ■ ■ 174. Then comes Neptune, the most distant planet of our system at present known, at 2,746 millions of miles from the sun, and taking 60,1 26 days to go round the sun. Its diameter is over four times greater than that of our earth, and its density is slightly less than that of Uranus. mi!^J-' ^ f-^ s-s" " '' ' ' ■ ^ 194. I have alre^#^iW^thJS'tlietealM:e of^ the sun from us is about ^i millions of miles. To^ [§n. ASTRONOMY. 83 every- ies the travel, ery life \k *ANCB ard the the ^un jtnpt to already rth, ajre f whif;!^ : henc^is liite hot equence its own planets odnj do sun IS a ; IS 500 jiilxm talfce ofti BS. To' % f go into the mode of measurement would lead ijs too far into mathematics for my present purpose ; but it may be stated here that knowing its distance and apparent size, we can proceed to find its diameter in this way. Let us draw imaginary lines from eithei side of the sun to the eve, as AB and A C, Fig. 39, ^ — ^ T — m *^,,Jt-t : Fig. 39. — How the size of the Sun is determined. CB representing the diameter of the sun, we find that the inclination of the two lines to each other is such that all lines drawn from one line to the other, as D£ or FG, are equal in length to y^ of their dis- tance from A, so also B Cis yjy part of the distance A By which we know is 9 1 millions of miles ; divid- ing this by 107 we get 850,467, which is the distance from B to C, or the diameter of the sun in miles. § III.—WHAT THE SUN IS LIKE. u. 195. There are not many observations th^ cftn. be made on the sun without the aid of a telescope iind dark glasses, and its intense heat and light render it dangerous to look at it without special precautions.' Ji you smoke a piece of glass over a candle, and look at the sun through it, it will appear to be a round bright object, because each part of it shines by its own light : unlike the moon, it is always round. This bright part is called the photosphere. In telescopes * The jrouog reader must not attempt to look at the sun through a small t^«> scope, for he or she may be blinded in the attempt. G 2 ,m 'ni U SCIENCE PRIMERS, r§iv. \\ black spots are frequently seen on its surface, and these, indeed, are sometimes of sufficient size to be ^ visible without the telescope. ^'^^^*"" "^''' ' 196. In the neighbourhood of the spots brighter portions than the general surface are seen : these are called faculse, and probably are immense banks of brighter vapours several thousands of miles long* If the spots and faculae be watched from time to time they will be found to be constantly changing their v^. shape. % IV.-^SUN.SPOTS. 197. Although the sun is so far away from ilSy , in consequence of its immense size and the violence of the forces at work, these spots are fine objects in -\ the telescope. I give a drawing of one (Fig. 40) sa'; large that several Earths might have been hurled ^^ ; into it 198. If these spots^ be observed and their positions carefully noted, and again observed one or two days afterwards, they will be found to have changed their position towards the west, and they will be seen to be gradually moving from the east side of the sun's disc to the west, where they will gradually disappear. ^ 199. Now, since all of these have the sattie mdtiBn in the same direction, it is evident that the surface of the sun is moving and carrying the spots with it, and if a well-marked spot be observed when passing oflf the disc to the west, it will be found about 12 days after to appear again on the east side and get to the portion ..here it was fi):st observed in about 25 days^ i\ ..'■n^V- \v;j; ASTRONOMY. tv N having in that time gone right across the disc and round the back. "^ ^: :-;-/" - — -i-i-s^- ^^r^^ 200. The surface of the sun has therefore moved round in 25 days, or in reahty the whole sun itself is turning round on its axis at this rate, carrying spots and faculae with it. j^ i. 201. Let us now see what kind of thing a spot is. If a pretty regular one is observed near the middle of "X, Mf ,l\h» ■J\k \j* ukku%j fiOll ^,,/Nf x^r -»,; Pk» 4»« — ^The Sun's coronal atmosphere. « • A ..^J- i c i i' then seen that the lighter vapours of the real fun are shot up into its outer atmosphere, called the coronal atmosphere, taking fants^stic shapes called prominences, and these prominences rapidly change. \nil 8 VI.— WHAT THE SUN IS 18 ABE 0«bb vV? .JI04. By analysing the light of the sun by meanS ot a spectioscope, an instrument that splits light up into its component colours, in the same manner as you have seen light split up into aP the colours of the rainbow by the glass drojps on chandeliers^ i^ tM«MMMi^MMMMiMMHHtai«UbMlMI 88 SCIENCE PRIMERS. »!. JU' It l,«« has been found that a great number of our metals exist in the sun, not of course in their metallic state, but in a state of vapour, the heat there being so intense that the metals evaporate as water with us does into steam. There are first of all, among the elements Uiat we know here, the ga^ h^cbrqgen, and : then vapours ol^^ipago^sium, calcium, sodium, iron, manganese, nielidt hvwft^, strontium, and v^' many more metals, besides probably two other gases, not yet foiawl on the «arth. altlo i^j^iaqmi a? r fidv/ wj 2Q5.,Sin€e^ as we hm^ ^een,,^the faun is so largely composed of gaseg^ you will not iie |pirprise4 that its density is mtich less than thati^ the earthy indeed, it is less than a quarter qI that ol oar pknet :i nzAi 206, I have been careful to dwell at some length on what il^fte ran. There are aboul: 3 jooo stars from the first to the siKt)^ magnitude visible at txnce ta the naked eye, and I there are over 29,000,000 "wsible in large telescopean ^^t j!ijl; You may h^vedsa noticed^ jCMi la-clear dark night,' ^ a zOi:^,! or bstnd of faijnfe light, stretching from the hori-^ii zpQ; on one side^jnearly over our heads to the horizoiir 00 the0di«r. Thisidscaflled the milky, way. 1. It is I con&posed pfian.^lmostinfialite number of smaU stars,! appaFently< so ddsd tc^ether as to form a ifiihinoudo mass -J and of the 20,000,000 telescopic stfirs^ probably 18,000,000 are ii;^, jtHe miljky way.,|| 4^ v of this gives us some little idea of the immensity of our universe, if we consider that it'is >not the rfeal close- ness of the Stairs* that we observe, b\it only their apparent closeness, placed, as they probably are, one almost behind the od^ier so as to be in nearly the same liteepf sigjit, and at a distance froua each other perhapS|8 as g^r^at £fi Hercules, . Hercules. iOn£ The Lyre. Ttie Swan. Cassiopeia Cpue Lady's Chair), Perseus,, .. ^^Cygnus. "A(\ ha « Cassiopea. vroffo ^ 4ur^at I IfMtHlWiintii 1*1; 99 SCIENCE PRIME J^S, [§iv, Serpmtaritts, Serpens, Sagitta, \^ ^^i^i Aquila. fJDeiphinus. Equuleus, .^^^. Pegasus. Andromeda. Triangulum, The Serpent-Bearer, •fhe Serpent. The Arrow. The Eagle. The Dolphijfi. The LiUle Horse. The Winged Horse. Andromeda. The Triangle. iViCamelopardalis* ri ijj^^he Camelopard. h'it'^n'Hnjr* mt, f. Canes Venaticu i-^ ^^ The Hunting Dogs. «^y^ r|y^ Vtdpecuia et Anser, The Fox and the Goosft ^ ^ CorCaroli. ' " '^tSkrles' Hearl:: w^^t) ^suv.. ..;.. lo B 1 7. The constellations visible in the Southern ? Heimsphere above llie zodiacal ipne^, K^iUedi th^.jc^ southern constellations, are : ,,r,. ^)^.j m ^gt)V Cetus. Orion. Eridanus. Lepus. Canis Major, Canis Minor, Argd Mtms. Aiiffydra. Corz/us, Centwrusf* Lupus, Ara. '^^ Corona Australis, Piscis Anstralis» Monoceros. Columba Noachi, Crux Australis, - ,iK .. ■ -^ The Whale. ' Orion. The River Eridanus. The Hare. The Great Dog. The Little Dog. The Ship Argo, The&iake, The Cup. The Crow. The Centaur, The Wolf. The Altar. The Southern Crown, The Southern Fish. The Unicom. v Noah*s Dove. The Southern Cross, A- ..VI ^ Afl T5?r-' 3 1 8. In ord^ to learn the positions of the various constellations and stars you will want a star-map or planisphere, and wiU algo requir9 §qv^^ f4end to point ASTRONOMY. 93 out to yovL some of the cliief ccwsteUations to begin with. I have indicated a few of these by Roman letters in the preceding lis^ f ^m t*..| .y, 219. The stars in each constellation are known by the prefix of some letter of the Greek alphabet, the brightest being called Alpha (a), the second brightest Beta O), and thei?, wheQ all die letters are used, they are numbered i, 2^ 35 so we can refer to a star as Alpha (a) Lyrse, the brightest sta?; in the constellation of the Lyre, Or (j3) Cygni, the §econd brightest in the Swan, 61 Cygni, and so on, so that every star can be named. In addition to these names the principal stars have other names, thus (a) Lyrss is also called Vega, a Canis Majoris is oUled Sirius, a Bootis^ Arc- turus, and so on. -.muMhin. § IV.— APPARENT MOVEMENTS OP THE ^ STARS. '>:. 'jff^ 4;^ .229. We saw in speaking of the earth that it was only a moving observatory, and that therefore we must distinguish the real motion of exterrw-l bodies firom that of the body on which we dwell. We may now return to this subject. Let i^s compare the eajth to a boat at sea ; imagine yourself in the boat ; then if it be suddenly turned round, all the ships in sight will, if you are ignorant of your motion, appear to go round you in the; opposite dicectign ; but it wpuU J^e highly improbable that afl the ships in sight §hoi;ld do so at the same rate, keeping, their relative posi- tiorjs to each other, so that you would at pnce find out that )four boat was moving, and not the ships. Just so, as we hav^ seen the earth turps round, anc| 94 SCIENCE PRIMERS, V. not tfie stars round us, 50, the daily motion of the star? ijB only apparent t ''ii ^ ,221. Now, Jet the^pQat pe ?:pwea round a ship. T)^ i:etative pcsitioos 01 t^e ship and the distant craft ch^ngje, the ship appears to move rpund you, passing between you and the other ships in succession. The same appefxance would be produceti were the boat |tp reffljaih ?till, and the distant ships to move round, it, bi^^ y^i^ wou}^ ^t once detect that |t was your own motion. Just ^o* with our annual revolution round th^ sun, the sun apparently passes over the stars ii^ succession, tjie stars whifrh -^e in a* line with the sun in summer being opppsite t^ him m wjbter.. ' ^ omBv ; 222. til the early day^oj^^iy^lronpmy th^se two ap-j parent motions of the stsu^J wfefe the, only ones known^j and in order to ascertain whet^ the stars were really 53^e^3a.^^»^< -m^ . m." ■ ^ .■ yf^ lfr$nt»BUjaQu^ I Vl.-MULTlPiiE STARS. ^^W^ 228. Not only have we such a proper motion along a path, but some stars go round each other. These^a^ce the nanie of double and multiple stars according as there are two or more moving round each other, as sihown in Fig. 43. ^ 229. Th^y are what is called physically connected ' with each other, being so cjpse^ that on^ revolves ^ icoui^d the other; just as we revolve round the sun, but instead of th* revolution being perform^ in a ypp; ASTRONOMY, 97 - the shortest known time of revolution or period of a ^t double star is thirty-six years. Up to the present i» time some 800 of these systems have been discovered. >>>.< .,^ ■ til oJ lyitl il591 ^* 43i*-C^blt of a Double Star. gllO.^ 230. Thf diiltances of the stars &om tis is so immense that if they had planets revcdving roraid tlpii these would be invisible with our most power- ful instruioents^ But it is prob^e that each star is the centre of a planetary system ; in the ifcs^ of close double staxsj therefore, the ptemiets of one star must be so near the other as to receive a considerable amount of light from it; in fact, the planets would have two suns, and, ift,^|t|e ^^| s^pving light of different colours. n -jj * fcjt" V- * "f^ ' ' : ' ; 8 viL-cmsTEEs and NEBUI,^. 231. Besides tlie scattered stars of which we have been talking, there are a numl)er ojf white patches in the s^y like litHe pieces of the Milky Way, a few of which are visible to the naked eye. When these are looked at with a telescope, some of thendi are seen to be veiy closely packed clusters of small stars; in some 9S » «l*«»»VnM»ft.--^ SCIENCE PRIMERS, f§ VII, the separate stars are seen with telescopes of loweJ power, while others require the highest telescopic means. Those in which the stars are easily seen, are called clusters, while those requiring high powers to see the separate starSi and those which still appear 1 ! fni. 44.^Tlie Ckntir in Hercules. of a cloudlike structure when the most powerful telescopes are brought to ^ear upon them, are called nebiJse. 232. We may therefore divide these objects into three classes : (i) the clusters, in which the separate stars are easily seen gradually merging into (2) the resolvable nebulae; and (3) the irresolvable ASTRONOMY. 99 vif. I * I > ; ■ II i j < ■» -^ % > nebulae. The spectroscope has shown .^ome ol these latter tQ be Q£.a nature diftbront Ji:i)uii«Laca.o«,»2 i^o^^i.? lection of atlar^v and SQiflt'^ife they aire wnlikc tkell tjttlBvloiisj'ni *^Ai ii) him ; gslwdait i©liiBvlo85ii 100 SCIENCE PRIMERS. [§ vni. 11 ; ,i \ y i ft" m ' 'm |i ih iij; li ' 111 I! ' J! ? * I i 233. Nor is this all : not only have we cloudlike masses which may be broken up into stars, and cloudlike masses which we know cannot consist of 3 true stars, but some stars, when closely exsunined, seem to be su ounded by a kind of fog, and these we know are not true stars, Such bodies are called nebulous stars. ? waiv -t:«34. Both the star clusters and i?ebula may from a different point of view be divided into two other classes : those which are very irregular in shape, like the Cluster and Nebula shown in Figs. 44 and 45, and those again which approach more to a globular ;ibrm* ,,....,,.:i.>... .e ^^^^ § VIII.-raE NATURE OF STARI^^;;^ 235. I have before told you that the stars are dis- tant Sims, but you are not to suppose that all of them are exactly like the sun j indeed, we have evidence that they are not. Among those which are very bright, some seem to have more simple atmospheres than the sun; that is, they do not contain all the elements staled in Art 204; and among those stars which are dimmer, and especially among those the light of which is reddish, the atmosnh »res seem fo differ in character fiom that of the sun, as ^^mark, J only say as //—such stars were colder than the sun. 236. Although the nebulae appear to be very dif- ferent from stars, it is possible that there is a very close connection between them, for it has been VIII. ASTRONOMY, lOI \-j ^thought that stars are formed by the coming together \fyi the materials of which the nebulae are composed, land that the planeta are formed in the process. ^rWhether nebulae are masses of glowing gas, or clouds tjof stones clashing together, and thus giving rise to a fluminous appearaiice, we do not know but the latter view is the more probable one. ^ ^^^ - ^i^ ui^j u -^ moi37- The idea to which I have referred, which 1 connects nebulae with stars and planets, supposes athat a nebula in its first stage is continually getting smaller and rounder, and that when it has done so perhaps sufl6ciently to give rise to the appearance of a nebulous star, getting hotter all the time, it leaves behind it, round its equator, as it still contracts, rings of vapour, something like the rings of Saturn (Art. 170) which eventually break and form a globular mass of vapour, which at last forms a planet. All the time the centre is getting more dense and hot, and at last, the rate of contraction still diminishing, it shines out like z. real sun, and thus goes on giving light and heat to those masses, now become cool and habitable, to which it originally gave birth. It thus shines, first, as a bright star, which afterward? becomes dim, and perhaps red, before the state of extinction is reached to which it must surely arrive ; for, do not forget, that any one mass of matter must in time cease to give out light and heat> whether that mass of matter be a coal in a fire or a star in the heaven. ;frf>: \rM £ ?;f,fii''s;- (X't'^i »!:i:t I02 SCIENCE PRIMERS, [§ii. 1 \\\ li tu i'! VI.— HOW THE POSITIONS OF THE HEa^- VENLY BODIES ARE DETEEMINEI>, AND THE USE THAT IS X*lADE OE § L^RECAP||mL^5PiON.~STAR MAPltW^^^^ ,■ ....,.-».....,r-.. , ■: ■'; .■ , j^frrrlo 238. I must now approach a different branch of my subject We have gone through the real motions of the eartL, moon, and planets, and more recently of the stars, and the apparent motions brought about by the real motion of the earth. We have referred to the nature of nebulae, suns, and planets^ and have thus got an idea of thq Earth's true place in Nature—* how it is a cool body going round a cooling star, bothn planet and star having probably resulted from th<^ condensation and consequent heating of a nebula^ :^ 239. I have also gr/en you an idea of th« starry heavens; how the stars — so-called fixed — ^have all been grouped into constellations, and lettered or numbered in the order of their brightness : aud how the sun by day, and the moon and planets by night, are perpetually changing their places among the «tars with the most perfect order and regularity. •'- n 240. I have now to ask your attention to tlie starr/f- vault, considerng the stars merely as things the posit/ ions of which have to be mapp(id ; and I want tail show you, first, how positions are determined, and then what use we make of them. ^ 241. If you were clever enough, you might be able to make a sketch-map of the positions of the stars, ASTRONOMY. 103 but for astronomical purposes the positions of the stars must be known with much greater accuracy than €ould be attained by such a rough attempt, and even if such maps w^ere perfectly accurate it would be very troublesome to have to refer to a star as being south of, or belowj a well-known star, and to the left, or west, of another ; another method of fixing their places for reference has therefore been adopted. A-^ '^'W&i^^iw'if '^t'fs ■^^'' Vfr^t § It— POLAR DISTANCE. !i' 142. We imagine the equatoi* and poles of our globe Extended outwards to the stars, just as their shadows would be cast by a light at the centre of the earth on the imaginaiy hollow globe on which the stars appear fixed (called the celestial sphere). The shadow of the earth's equator thus, becomes the celestial equator, and we measure north and south to it in degrees from the shadows of the poles, calling this distance polar distance. ^" • j; ,.. 1 243. In this way we can say which star or which part of the sky is exactly at the pole, because it will have no motion. Get yoiu: orange and stick a pin in it at each pole ; if you turn the orange round, the pin will still point to the same place. This, then, will be o** polar distance. Now, with a telescope furnished with circles, we can find tWs spot in the heavens, and turning the telescope 10° from this spot (which we can easily do by means of the small circle fixed to it, because you have already seen that all circles big or little are divided into 360*', Art 126) we can detei liiine those stars which have 10° polar distance, then 20% 30°, and so on, till we come to 90", which of 104 SCIENCE PRIMERS. [§ ni. course marks the position of the Celestial Equator-^ that is, the line in the heavens which lies exactly half-way between the north and south poles, as th^ terrestrial equator does on the earth. 1 ^^^^ ^^ noiliaoq ov^ ,QLk nioii d foflfi E.k cnott ?Mommh t tp, tf*f>jp § in.—POLAR DISTANCE IS NOT SUFFICIENT. 244. In this way, then, we can determine the pojar distance of all the stars ; but you will see at once that a multitude of stars may have the same polar dis- tance, for we can stick a whole row of pins in the orange, so that all shall be the same distance ^^ the pole of the orange marked by another pin. . " ^ 245. It is necessary, then, to distinguish these apart somehow. Do not forget that the question is to ii^ 'Wl 3V"£fl ion ■ At C 6 am n — r-n ?-ir ' ^ 1o aDSiq -i M • — u iij. ! u O would you fix the position of a dot on a piece of paper? Let us see. Take a sheet of paper :/4 -5 C/>^ Fig. 46, and stick a pin in or make a dot -S 6ri it Now let us see hov/ we can state its position: divide the side AD into, say, 10 equal parts, and AB into, say, the same number; then on joining EG III. ■inm ,. ASTRONOMY, 105 fix of and EF^ you will see that E is 4J divisions from ^e line AB measured along ADy and is 2 J divisions from AD measured along AB, so we can fix the position to this point E at once with reference to the edges of the paper. So also if you were asked to place a dot at 7 divisions from AB and 6 from AD, you Would draw a line HI from the seventh division on AD and another KL from the sixth division on AB^ then the point M where they cross will be the place 246. Now mark well that it is not enough to say that E is 44 divisions fix)m AB, because there might have been a whole line of pins or dots at that dis- tance from AB, and that it is not enough to say tiiat E is 2 J divisions from AD, because in like manner there might have been a whole line of pins or dots at that distance. 247. Mark well also that the moment we have two sets of measures at right angles (you have not for> gotten, I hope, what that means) to each other, we can state the position of a pin or dot on our piece of paper with the greatest accuracy. j 248. So it is with the stars. I have already made you acquainted with one set of measures, that which begins at the poles and measures the distances of the stars from the poles, or, what comes to the same thing, the distance from the equator, because when we know the number of degrees a star is from the pole, the dif- fiurence between that number and 90° will give us the ^istarce from the equator, as of course the equator is 90° from each pole. In the next diagram, Fig. 47, I have drawn the equator and straight lines 10'' apart between it and each pole. io6 SCIENCE PRIMERS. [§iv. t iitjtrtrtfi'ff'--"* ' ' I ' '" ^"^ "^ *"*' *" "^^ "" ! I - II ..■-;■■:■ i .. . ^'\ . § IV.~RIGHT ASCENSI0K5' ^^^:^ 249. Evidently therefore, to make our statement of ft sWs position complete, we want another line at light angles to these. Now get your orange, and stick a row of pins in it all round to mark the equa- tor -<4 B Fig. 47i Next, stick another, row of pins in at right angles to the first row CD, This second row will take the shape of a second circle of pins, passii^ over the poliss of thie orange, and cutting 4})^ equat^ in two opposite points. , , ? : , 25a Now the equator, and the row of pins which represents it^ can only be in on» place ox^ the orange, that is half-way between the two poles; l-'V ASTRONOMY. 107 i/Vff-i* fT -;sr) My '% ^t But you may make the, secpud circle wherever you choose, and in fact you may suppose an infinite number of such circles, all of them at right angles to tne equator, all cutting it; in two opposite points, all passing through the poles; of course we can imagine them i"^ or 10°, oj: any other number of de- grees apart; if we imagine theip to be 15° apart, then as the heavens aj^ear to revolve round the earth in 24 hours, one of these circles will pass over a place on the earth every hour, because 15° X 24 = 360°. 251. But we, have not; yet got over our difficulties. All these circles are alike ; we must therefore choose one to measure frpm, to^, represent ^e .equator, as it were. Yqu will perhaps think that the first will be n^ade to passi through , the brightest ^^ ^ This is not so ; one of the two points of the celestial equator which lies exactly in the plane of the ecliptic (Art. 67) is chosen. Tl^is point is, ^palled the first point of Aries. m y i:t 252. This being detemuned on, all the astronomer has to do is first to regulate his clock so that the stars shall appear to travel round the earth in exactly 24 hours ; to let it show o*" o" o", when this imaginary circle, which passes through the first point of Aries, passes what is called the meridian, that is a fixed imaginary circle passing from north to south overhead, and to note the time when each star also passes it. As each star, whatever tJe its polar distance, passes this line, the clock, if it goes correctly, will show its distance in time from the first point of Aries;. Thus we say fji^tjhe Right Ascension of the brightest star (ft) in the Bull is 4^ 28'*; of the brightest star in thfi, Virgin, 13^ 18"™, and so on. !..■ .,mtt¥<0mm w io8 SCIENCE PRIMERS, [§vi. II I f, mtHi iu p^i % y.r-RECAPITULATION. il w I a53. If yw have undetstotfd this ^o" will thow t the place ot a star is stated or defined : — i JFirst — By its distance in degrees from the pole: This is called ^ts poUr distance; from which (as stated in Art. 249) we can easily determine its dis- tance from the equator, called its declination^ )i| ^A% And Secondly — By its distance^^in time from the g^eat circle which passes through the £urst point of Aries. This is called its Right Ascension. bod 1254. The positions of all star^ have thus been determmed, and furtlier, we cjan calculate what position among the star9 the sun, inoon, or ^ny of lihe pla^eta ^l^pccupy^t apj^lnatanl 1255. Thi^ if 0|ie of the Ws^tusfftilire^ults of As^ tronomical Science, for it enables u$ to map the sub face of the eairthi and also enables the traveller in the trackless waste, or the mariner out of s%ht of landf t^^]^ opt exactly where he \&m thati$iirface»w uq\ ,f>B3rf 1UK>% 19VO b988Bq l&tZ lElODltSBq ifidJ \l ^^iS^ Let tis S^elpn how w6 can fixri^»o§itio^,pf any place o»|fne earth. If you were asked to t^ knyone wfeeffe' a neighbouring tow^ or village was, you would probably say so many miles away, ^lid $,long a certain road, or in a certain direction, ^W. of yoof hbus4 This answers very well for d'-f %] ASTRONOMY, to^ distances, but it would never do to refer all places to this distance and direction from your house, or from any other one place. If the earth were flat we could uae tile method referred to in Art. 246, but as the eieuth is not flat, we do this ; we measure from the equator towards the pole in either hemisphere, ahd if you refer to a globe you will see that there is a number (tf circles drawn at equal distance apart between the poles and die equator. These circles are called' parallels of laCitade4^^^ '^^ ^ i^..w^^..o ui.xi 257. Remember, that the positioHsrof the heavenly^ bodies have been determined with reference to the earth's pole and by means of its rotation. Now, if yoi^ will think a HtlEle, ydu Wrll see that if dtere were f stl^ known to be of ci^ noi^ polar distance, that star wdiil^ be exactly over your head if you were at the hdftS pole, and therefore you would know yoii ^ti'i a^ the pole if that star appeared fixed exactly over your head. If there were a star known td W of 90^ polar distance, that star would be exactly ovei^ your head itf you were at the equator; and theifcfbr^ you would kno^ that you were at the equatot^ if that particular star passed over your head. 258. Similarly, for any place north or south of the eq^kter, we can determine the distance in degrees of that place from the equator, by observing which star, )r other heavenly body the declination (Art» 253) of (fiK^il^ kpown^ passes overhead. And this is the ling of the equator^ and of the circles parallel to if,^'|^ou see in maps and globes. An observation, th^e principle of which I have stated, must have be^ itmde before the positions of any places were laid! down, Ithus, in maps, you will And the distance of 110 SCIENCE PRIMERS, [§ VII, I I London from the equator shown as 51^° N, be- cause the star y Draconis, with a north declination of 5i§°, passes exactly over London. 259. This distance from the terrestrial equator is called latitude, the distance from the celestial equa- tor being called declination (it is a pity that the same word is not. used for both)^ and w^ '-^ 8 VII. itfv M A ASTRONOMY. MI3 ange sding pins, vatdi d lit wich; :e the repre- is tnll ieedle ginary ry star M of ime as ve the no! mwich, As the >t, it is cip iittd th^t which 2 lamp, time, setiwich jsenting tie clock .^, let us e of one laces of of pins ' J Dyii37o. Now let the lamp represent the sun. The sun ^prings local time to a place, because it is 12 o'clock (near enough for our present purpose) at a place when ,lthe sun is south or crosses the meridian at midday. ■J If therefore I have this local time and Greenwich time as well, I can tell first whether I am east or west of Greenwich, and then how far east or west. If when with me it is 10 a.m. it is is (noon) at Greenwich, then I am situated to the west of Greenwich, and the earth must turn for two hours before I am brought .under the sun; if it is 2 p.m. with me when it is 12 (noon) at Greenwich, then I am to the east of Green- wich, as I passed under the sun two hours ago. Such [a Ciifierence of time of 12 hours ss 180^; of 6 hours = 90** east or west ; of 3 hours, 45° east or west, and so on; so that it is immaterial whether we reckon longitude in degrees or hours, for since there are 360 degrees or 24 hours into which the equator is divided, each hour corresponds to 15°. We also express the longitude of a place by its distance '^ast of Green- wich in hours, so instead of calling a place twenty- jfliree hours west it is called one hour east, ^i^i'^n:?^ ^ri^ ffn 271. In practice a difficulty arises in finding out at a distance from Greenwich the exact time^ at Green- wich. A great number of ways have been tried, in order to let it be known at one observing station what time it is at the other. Rockets have been sent up, guns fired, fires lit, and all kinds of signals made at fixed times for this purpose; but these, of course, only answer for short distances, so for long ones care- rfuUy-adjusted chronometers had to be carriM from one station to the other, to convey the correct time ; but now, when telegraph wires are laid firom one place m SCIENCE PRIMERS. [§I. to another, as fronx England to America, it iis^easy to let either station know what time it is at the other. For ships at sea chronometers answer well for a short time, but they are liable to variation. i^-g72. There are certain astronomical phenomena whose instant of occurrence can be foretold, and which occur so far away from the earth that they are visible over a great part of its surface at the same moment of time ; these are published in the Nautical Almanacs, such as the eclipses of Jupiter's moons, and the position of our own moon. Suppose that an eclipse of one ol Jupiters moons is, to take place at i^l'.M. Greenwich time, aad it is observed at a place at 2, P.M. of their local tirnjC, /.^., two hours after the sun had passed the meridian, then manifestly the dock at Greenwich is at i p.m^ while theirs is at i* Ejsi., and the dJJSference of local time is one hour, and the place is one hour or 15° east of Greenwich. Xf^,; however, the eclipse was observed at .12 noon, then the place must be one hour west of Greenwich*. ^^ VII.— WHY THE MOTIONS OF Tttfe^'^EAr ^ VENLV BODIES ARE SO REGIJLAI^. ' ; 273. We have just seen that the stars are so useful toman because we can exactly calculate in what part of the heavens they will beat any future time. Now of course if their motion or our motion were irregular, this coi|ld not be done. Before I complete my task then L must attempt to explain to you how it is that we are enabled tQ foretell. the movements. ASTRONOMY, "S c »•¥• 274. This brings us to the more mechanical part of Astronomy, the laws of the motions of the heavenly bodies. The ancients believed the earth to be at rest and the sun and planets to revolve round it. This idea, however, gave way for the correct one which has been stated, and then came the question, Why do they so revolve ? It was first supposed that the planets were carried round in a vortex or whirl- pool of some kind ; and it was afterwards shown that the planets revolve round the sun and the moons round their primaries, not exactly in circles, but what are called ellipses, having the sun not quite in the centre. Newton showed that on mechanical princi- ples they ought to do so, and I must try to show you ^275. You have doubtless often seen a ball or stone thrown up in the air and fall again to the earth. Did you ever ask yourself the question, why does it fall? Probably not; but if you were asked you would probably answer, " Because all things that are heavy fall to the earth ; " and so you would get out of the difficulty, but only to get into another. Why are things heavy? is the next question. The answer is, that all substances attract each other in the same manner as a magnet attracts iron ; so one stone attracts another stone, but with very small force, and the earth being an immense mass of different substances attracts all things on it with such a force that the attraction of one stone on another is inappreciable in comparison. 276. The weight or gravity therefore of an3rthing only means the force with which the earth attracts it, and causes it to gravUate towards itself. VSBSB9SUSM ii6 SCIENCE PRIMERS. [§n. 277. Now the attractive power of bodies is in pro- jTOrtion to the amount of matter they contain. For instance, if the earth were doubled in size, still being made of the same materials, it would attract every- thing on it with double the force it now does, and consequently everything would weigh double its pre-^ sent weight — so that then our legs would have to carry as much weight as if there were a person on our back continually. Also if we double the quantity<> of matter attracted by the earth, the force with which^ it is attracted, or its weight, is also doubled. For instance, a pint of water weighs one and a quarter- pounds, two pints therefore, weigh two and a hatf . pounds. • ., 278. I have before (Art. 135) made use of the words quantity of matter or mass. A pint of lead., contains a greater quantity of matter or has a greater mass than a pint of water, and the word mass is practically only another word for weight so long as we are on the earth; but a pouna weight here would weigh over two pounds at Jupiter, although the quan- , tity of matter or mass is unchanged. So in dealing with the weights of bodies under different attractions we must use a word expressing a constant quantity of matter. 279. If our earth were doubled in size, a pound weight would still balance another pound weight in the scales, for both would have their weights increased really to two pounds ,• so we must use some other means to determine anyalteration of the force of gravity. - 280. A spring can be arranged so as to answer the purpose, as it is not altered in any way by gravity; but •rff * "1 OT m 'E^ ~,i M t? ASTRONOMY, "7 the most accurate method is to ascertain the distance through which a body falls to the earth in a certain time, usually one second, since the greater the attraction the quicker will be the fall j at the surface of the earth a body will fall, in a vacuum or space without air to resist it, i6 feet in one second, and at the end of that second its velocity is 32 feet a second, — that is, if the force of gravity ceased at the end of the second it would go on through 32 feet in the next second. -^^m>U^*^''mk"'i^ ~^''^^-%\K:?.^^^^^^ -r. ■ -., :, ;, 281. The force of gravity at the earth's surface is therefore represented by 32. On the surface of Jupiter the force of gravity is 2\ times that of our earth and is represented by 78, meaning that in one second a body allowed freel;^ to fall would attain a velocity p of 78 feet a second. ^ ^^ -^jstrciuip rtuwi^ •* «ai«. § II,— GRAVITY DECREASES WITH DISTANCE. ' ^ . . , ;■ ;;;^ :_;:,r ■ ^,i,:f..«r \,,m\m% ^ ji ind i . iiiiA^a ■■ 3ifc?-' jro a-li. 282. I have already told you that the weight of>^^ anything on the earth means the force with which the earth attracts it. I have now to add that this force Qot the same for bodies at different distances from earth. 'r 1% .: :^. Those of you who have had a magnet iii your hands have probably noticed that pieces of iron are attracted the more strongly the nearer they are to the magnet ; this is easily seen by laying a needle on the table and sliding a magnet towards it, when you will see that at a distance of a few mches the needle is not attracted with sufficient force to overcome the triction of its rolling on the table, and the magnet tfi8 r i i ii j i<» > <»ii f ii »» ii > i« SCIENCE PRIMERS. [§ ni. has to be moved nearer to it until the force is suf^ ficient to ov^ercome the :iesistartce, when the needle rushes to the magnet. /^jy''^-^n:,:^:--^*'f^,^\x^^ 284. It is just the same with gravitation, the further a body is away from the earth the less it is attracted; and Newton found that the force of gravity at double the distance was not half, but half of a half, or one quarter; at three times not a third, but a third of a third, or one ninth, and so on ; so if the distance be increased to eight times, we have to multiply eight by itself, or what is c. l square it, making 64, and placing I over it, maku ^^ showing that the attraction at eight times the distance is only one sixty-fourth of what it was originally, y .1 i ; ? hi^ » « « § III.— HOW THIS EXPLAINS THE MOON»S PATH ROUND THE EARTH. , 285. Newton tested this by the motion of the moon in the following manner: The moon, as we have already found, revolves round the earth ; hut we have not seen yet why it should do so. Now, however, we are prepared to find that it is held in its nearly circular orbit by the attraction of the earth acting on it as a sling does on the stone, preventing it from flying off, as it would do if the string of gravity were cut, just as the stone flies away in a straight line when the sling is released, 286. Let us consider this with the help of the diagram, where JE represents the earth and MB A the orbit of the moon ; and let us suppose the moon to be at M; then if gravity ceased to act, the moon would continue on in the same straight line that it was moving' III. suf- ;dle 3mi ther j-j ted; able one of a be : by * and ction th of H .-'■ N»S moon have i have er, we ircular t as a ngoff, just as e sling of the ?^the oon to I would moving T Aii^l ASTRONOMY, '!■■ V 119 mmm ■««>***«^uc»i ni'i fiinM-»y-f in at the time gravity ceased to act, and would go on towards N; and in one second it would get, say to M^ but by the action of gravity we find the moon actually at B^ showing that the earth's attraction has had the effect of drawing it from M' to By and since we know the dimension of the moon's orbit, it is only a matter of calculation to find the distance from M' to B through which the earth draws the moon in one second| which i5,a.litile uad^. Qne-eighteenth. of an inch. ^^. \ . • iO'. v'^pm aiDO fr,.f-* ^^ -V ■ miH^ zmmh \c. .i^vx^'t;-^ 1^ >Ji;. ili: i|'l4"3 feworfa; ^*f^ i^tii liom ^iAi itU iWJO't Hi t?t'' -- i^lk j£'iii m ''-^-^ ^i'l) rf S^.^ir;|rr>f.f^'>t4t:| biifO^J S10^''J'Ii?rfl fell*. ,1fi^^- VK J'-.yf'-. vnOfii it ^( ft ^5fO to If r, > r. », ■cf Mmi^- ■t