272 Mifcellanea Curio fa. 



when the Moon's Apogee is any where but in 

 the Otlants, this Equation grows lefs, and is 

 moftly at the fame diftance between the Earth 

 and Sun, as the Sine of the double Diftance of 

 the Moon's Apogee, from the next Quadrature 

 or Syzygy, to the Radius. 



This is to be added to the Moon's Motion, 

 while her Apogee paffesfrom a Quadrature with 

 the Sun to a Syzygy ; but this is to be fubtra&cd 

 from it, while the Apogee moves from the Sy- 

 xygy to the Quadrature. 



There is moreover another Equation of the 

 Moon's Motion, which depends on the Afpecl: 

 of the Nodes of the Moon's Orbit with the 

 Sun : And this is greateft, when her Nodes 

 are in OFtants to the Sun, and vanifhes quite,, 

 ■when they come to their Quadratures or Sy- 

 zygys. This Equation is proportional to the^ 

 Sine of the double Diftance of the Node from 

 the next Syzygy, or Quadrature ; and at grea- 

 teft, is but 47 leconds. This muft be added 

 to the Moon's mean Motion, while the Nodes 

 are patting from their Syzygys with the Sun, 

 to their Quadratures with him ; but fiibtra&cd 

 while they pafs from the Quadratures to the 

 Syzygys. 



From the Sun's true Place, take the equated 

 mean Motion of the Lunar Apogee, as was 

 above fhew'd, the Remainder will be the Annu- 

 al Argument of thefaid Apogee From whence 

 the Eccentricity of the Moow, and the fecond Equa- 

 tion of her Apogee may be computed after 

 the manner of the following (which takes place 

 nlfo in the Computation of any ether intermediate 

 Equations \ 



Let 



