Miftellanea Curiofa* 0 J g 



Tab. 3. Fig. 6*. Let T reprefent the Earth' 

 TS, a Right Line joining the Earth and Sun> 

 TACB, a Right Line drawn from the Earth 

 to the middle or mean Place of the Moon's Apo- 

 gee, equated, as above.- Let the Angle ST A 

 be the Annual Argument of the afurefaid Apo- 

 gee, T A the leaft Eccentricity of the Moon's 

 Orbit, TB the greateft. Biffed* AB in Gj 

 and on the Centre C, with the Diftance A C 

 defcribe a Circle A F B, and make the Angle 

 B C F = to the double of the Ar nual Argument. 

 Draw the Right Line T F, thatfhallbe the Ec- 

 centricity of the Moon's Orbit \ and the Angle 

 B T F, is the fecond Equation of the Moon's 

 Apogee required. 



In order to whofe Determination, let the mean 

 Diftance of the Earth from the Moon, or the 

 Semi-diameter of the Moon's Orbit, be 100000; 

 then (hall its greateft Eccentricity T B be 667 8^ 

 fuch Parts ; and the leaft T A, 43319. So 

 that the greateft Equation of the Orbit, vi%, 

 when the Apogee is in the Syzygys, will be 7 

 degrees, 39 minutes, 30 feconds, or perhaps 7 

 degrees, 40 minutes, (for I fufpedl: there will be 

 (bme Alteration, according to the Pofition of the 

 Apogee in Cancer and Capricorn.) But when it is 

 Quadrate to the Sun, the greateft Equation a* 

 forefaid will be 4 degrees, 57 minutes, 56 fe«? 

 conds j and the greateft Equation of' the Apo- 

 gee, 11 degrees, 15 minutes, 4 (econds. ; 



Having from thefe Principles made a Table 

 of the Equation of the Moon's Apogee, ..and 

 of the Eccentricities of her Orbit to eaglv de- 

 gree of the Annual Argument, from whence 

 the Eccentricity T F, and the Angle BTF 

 (vi^. the fecond and the principal Equation of 



T the 



