Viewing page 478 of 504

This transcription has been completed. Contact us with corrections.

x/SL[[squared]] to t/TL[[squared]]; as they are really in the Solar System.  These inestimable Advantages cannot but seem very great, and lead us to excellent Conclusions.

9.  In the Sphere OLP, the Point P is the nearest to the Sun S, and to the Earth T: and the Point O is the furthermost from them.

10. Let SP be called y, [[underline]]viz[[/underline]]: the Distance betwixt the Center of the Sun and the Perihelic or Perigee of the Sphere OLP.  Let the Radius PC or CO of the Moon's Orbit be called h. And let CT, or the smallest possible Excentricity of the orbit of the Moon, be called E for the Winter Season; and be called e for the Summer Season; and be called o, if when the Centers of the Earth and of the Sun are at their mean Distance, we reduce the Orb of the Moon to a Sterographic Orb.

11.  Thus, for any Time when the Center of the Moon may be supposed to describe its Orbit upon the Spherical Surface OLP, or when that Orbit may be made equivalent to an Orbit described upon the Sphere OLP; or when the Center of the Moon touches the Sphere OLP; The Distance of the Sun in Feet, or in Parts of the Radius of the Orbit of the Moon, may be found, and by consequence the Parallax of the Sun also, by saying only, As either of the two smallest possible Excentricities CT, [[underline]] viz [[/underline]]. E or e; Is to the Radius CP or h of the Orbit of the Moon:  So is that Radius CP; To hh/E or hh/e, that is, to the Distance CS, or cs, betwixt the Centers of the Sun, and of [[y to the power of e]] Orbit of the Moon; expressed at your Choice, either in Feet, or in Parts of the Radius CP.

12.  And those two smallest possible Ex[[^c]]entricities CT, or E and e, are to one another as
1016
[[end of page]]