66

Use of the Globes. jthe other below it; and the E s

d

an oblique Direct' 011 ^ . 'I’l'jJ

: have formerly 0 -1

to the Earth’s Orb . e ,

tator will fee the Star inin the Perpendicular, as we

is, if GF be a Tangent to the Earth’s L £.!]jpti £ Aand B E perpendicular to the Plane of the N ^ 0the Point B, then while the Earth moves thr® .indefinitely small Arch G B, a Star at E ^to move from E to e,. or to be in e when

WiJ' -yvtl-e ^

$

arrives at B. -„t

22. Now since the Distance.S B is but a \°c 0 \\<ff’

respect to the great Distance S P of the Star, l£ fo ‘0that we may refer the Spectator from the f eV s v jiig 1 jA, B, C, D, to the central Point S, for ohfeNPhœnomena of the Star at P, which will notthereby. Therefore if c a be parallel to A C> „ h '0make the Angle P S a equal to the Angle E ^ ^plain the Star P must appear in et, in the Dj re £ f e efl ‘Also when the Earth is at D, the Star will t'the oblique Direction S c at c, the Spectator . ,

ferred to S. .

23. For the like Reason, viz. because b ** spg el> Jor alike situated in respect of D B, and to the r ihin D and B, therefore the Star at P will a ?L-jjiS? 1 5and b when the Earth is at C and A ; and st> j e (cs'sSpace of one Year the Star P will appear t° ^id 1small Circle a de b, supposing the Star in the rjistd 1of the Spectator; but if the Star be at an ¥ eC o 0 e 3from the Zenith, the said small Circle wiH °

Ellipse, as in Fig. 7. c^s °.t

24. These small elliptic Motions of the P<easioned their Declinations to vary, and a a t b f\</tances from the Poles of the World, and *■

Space of 20" | on one Side and on the °s e (s lCl ,’sthis could not happen on any account of w ^ Al

because the fame thing was as well observe ^el>

near the Zenith, where there is no Refract 1where situated. Nor could it result from '

of the Earth’s Axis; for that would haveequal Distances of the Stars on opsPole unequal, which never happened

m a ‘

25 '