Galilei, Galileo
,
The systems of the world
,
1661
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bed circle ſhall be in the line F G, which let be the point I; and
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becauſe that of ſuch lines as are drawn from the point G, which
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is not the centre, unto the circumference of the circumſcribed
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circle, the biggeſt is that which paſſeth by the centre, G F ſhall
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be bigger than any other that is drawn from the point G, to the
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circumference of the ſaid circle; and therefore that
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rence will cut the line G H (which is equal to the line G F) and
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cutting G H, it will alſo cut A H. </
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<
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>Let it cut it in L, and
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joyn the line L B. </
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<
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>Theſe two angles, therefore, A F B and A L B
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ſhall be equal, as being in the ſame portion of the circle
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cumſcribed. </
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<
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>But A L B external, is bigger than the internal H;
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therefore the angle F is bigger than the angle H. </
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<
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>And by the
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ſame method we might demonſtrate the angle H to be bigger
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than the angle E, becauſe that of the circle deſcribed about the
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triangle A H B, the centre is in the perpendicular G F, to which
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the line G H is nearer than the line G E, and therefore the
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cumference of it cutteth G E, and alſo A E, whereupon the
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poſition is manifeſt. </
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<
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>We will conclude from hence, that the
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ference of appearance, (which with the proper term of art, we
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might call the Parallax of the fixed ſtars) is greater, or leſſe,
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cording as the Stars obſerved are more or leſſe adjacent to the
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Pole of the Ecliptick, ſo that, in concluſion of thoſe Stars that
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are in the Ecliptick it ſelf, the ſaid diverſity is reduced to nothing.
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</
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<
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>In the next place, as to the Earths acceſſion by that motion to,
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or receſſion from the Stars, it appeareth to, and recedeth from
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thoſe that are in the Ecliptick, the quantity of the whole
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ter of the grand Orb, as we did ſee even now, but that acceſſion
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or receſſion to, or from the ſtars about the Pole of the Ecliptick,
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is almoſt nothing; and in going to and from others, this
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rence groweth greater, according as they are neerer to the
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tick. </
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<
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>We may, in the third place, know, that the ſaid difference
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of Aſpect groweth greater or leſſer, according as the Star
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ved ſhall be neerer to us, or farther from us. </
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<
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>For if we draw
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nother Meridian, leſſe diſtant from the Earth; as for example,
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this D F I [
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in Fig.
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7.] a Star placed in F, and ſeen by the ſame
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ray A F E, the Earth being in A, would, in caſe it ſhould be
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ſerved from the Earth in B, appear according to the ray B F, and
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would make the angle of difference, namely, B F A, bigger
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than the former A E B, being the exteriour angle of the
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gle B F E.</
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An Indice in
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the fixed ſtars like
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to that which is
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ſeen in the
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nets, is an
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ment of the Earths
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annual motion.
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The fixed ſtars
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without the
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tick elevate and
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deſcend more or
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leſſe, according to
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their diſtance from
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the ſaid Ecliptick.
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*
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i. </
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<
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>e.
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of the
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cliptick.</
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The Earth
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proacheth or
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deth from the
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ed ſtars of the
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cliptick, the
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tity of the
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ter of the Grand
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Orb.
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The ſtars
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er to us make
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greater differences
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than the more
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more.
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<
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>SAGR. </
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<
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>With great delight, and alſo benefit have I heard
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your diſcourſe; and that I may be certain, whether I have
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ly underſtood the ſame, I ſhall give you the ſumme of the
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cluſions in a few words. </
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<
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>As I take it, you have explained to us
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the different appearances, that by means of the Earths annual </
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