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is neither in the Pole nor Plain of the Ecliptick, will 
feemto deferibe about its true Place a Figure, infenff 
bly different from an Ellipfe, vvhofe Tranfverfe Axis 
is at Right-angle to the Circle of Longitude palling 
through the Stars true Place,, and equal to the Diame- 
ter of the little Circle deferibed by a Star fas was 
before fuppofed) in the Pole of the Ecliptick ; and 
whofe Conjugate Axis is to its Tranfverfe Axis, as the 
Sine of the Stars Latitude to the Radius. And al- 
lowing that a Star by its apparent Motion does ex- 
adrly deferibe fuch an Ellipfe, it will be found, that 
if A be the Angle of Pofition (or the Angle at the 
Star made by two great Circles drawn from it, thro* 
the Poles of the Ecliptick and Equator) and B be 
another Angle, whofe Tangent is to the Tangent of 
A as Radius to the Sine of the Latitude of the Star ; 
then B will be equal to the Difference of Longitude 
between the Sun and the Star, when the true and ap- 
parent Declination of the Star are the fame. And if 
the Sun’s Longitude in the Ecliptick be reckoned 
from that Point, wherein it is when this happens ; 
then the Difference between the true and apparent 
Declination of the Star (on Account of the Caufe I 
am now confidering) will be always, as the Sine of 
the Sun’s Longitude from thence. It will likewife be 
found, that the greatefl Difference of Declination 
that can be between the true and apparent Place of 
the Star, will be to the Semi-Tranfverfe Axis of the 
Ellipfe (or to the Semi-diameter of the little Circle de- 
fended by a Star in the Pole of the Ecliptick) as the 
Sine of A to the Sine of Bi 
If the Star hath North Latitude, the Time, when 
its true, and apparent Declination are the fame, is be- 
fore 
