233

to

to Lecture XI.

ipp * C ^* me describing it; whence it^ e -^ art os Time to be added tojdereal Day, to ccmpleat the Solar2 ’ 1S a hvays variable.

^tie ^ HE olher Part of the Equation of6 ( a ' a d most considerable) is that whichOf ^ sto m f iie p] ane of the Earth’s Orbitbeing inclined to that of theh e ^ tor or Plane of the Diurnal Motion;Of T^tain which, let v v$ be a SemicircleEcliptic, and y PI * of the Equi-^ ' S the Centre of the Sun, and A\ ^ ^be Earth in the third Quarter ofAstatic; hf the MeriTan pasting^b the true Sun S, and .its apparenttic ‘

Y

^ I in the first Quarter of the Eclip-ar.

Suppose, now, the Motion of the- 111 every Respect equable, and first|? bit out from £ , and proceeded inin a given Time to D, the SunV ^ apparently describe in the same TimeJtye j of the Equator cy> I. Again, sup-out from the same Point andd 0c j t E same Time with the same equablebi the Ecliptic, it would arrive to<y, ^ so that the Arch ~ A = ^ D,'Mtjj ^ <v C. Then ’tis evident, as therev olves about its Axis from West to

East,

PlateLXIV.Fig. 5 ,