[ 2i 3 
indeed with an equable Motion j but in the Ratio 
of the Sine of the Diftance of the Moon’s Node 
from the Beginning of Aries . For if the Node be 
fuppofed to have gone backwards from Aries 30'% 
or to the Beginning of Rifces j the Point, which 
reprefents the Place of the true Pole, will in the 
mean time, have moved in the little Circle, thro' 
an Arc, as AO , of 30° likewife : and would there- 
fore in EfFed have approached the Stars that lie in 
the Equinodial Colure and have receded from 
thofe that lie in jP— , 4 , which is the Sine of 
30° to the Radius AR. For if a Perpendicular 
fall from O upon R A, it may be conceived as 
Part of a great Circle, pafTing thro' the true Pole 
and any Star lying in the Equinodial Colure. 
Now the fame Proportion, that holds in thefe Stars, 
will obtain likewife in all others; and from hence 
we may colled a general Rule, for finding how 
much nearer or farther, any particular Star is, to or 
from, the mean Pole, in any given Pofition of the 
Moon’s Node. 
For, if from the Right -Afcenfion of the Star , we 
fubftrabl the 'Diflance of the Moons Afcending Node 
from Aries ; then the Radius will be to the Sine of the 
Remainder , as 9", is to the Number of Seconds, that 
the Star is nearer to, or farther from the Tme> 
than the Mean Role . When that Remainder is lefs 
than 1 8o°, the Star is nearer to the True, than to 
the Mean Pole ; and the contrary, when it is greater 
than 1 8o°. 
This Motion of the true Pole, about the mean at: 
R, will alfo produce a Change in the Right Afcen- 
fons of the Stars, and in the Places of the Equinoc- 
tial Points ; as well as in the Obliquity of the Eclip- 
C 2 tic : 
