Appendix

th*

will be in the Position m d, parallel toformer M D. But ’tis plain, the ^ ellsl Jl0 rm d is not yet directed to the Sun> , ^will not, till by its angular Motion hattained the Situation e f, describesAngle e B m — B S A; whence itthat all the Solar Days are long er Jthe Time of one Revolution, or S l

Id ay , . p]asl e ■

22. If the Earth revolved in the

of the Equator, and in a Circle about ^Sun, then would the Angle A 8 B, , sconsequently the Angle e B m be ^of the same Quantity, and therefore ^Time of describing the said Angle * ^would always be equal, and so all th^ ^Days would be equal among them * eBut neither of these two Cases havein Nature.

23. For by the Earth’s Theory, t° u . ^on the nicest Observations, the Orbh \Dllipjis, and therefore (as we have f o(her annual Motion cannot be equa>V'^the Angle A S B described in the saute

of Time will not he equal; f° r ra ^.;[1Aphelion, the Velocity of the Eai'tbbe less than in the Perihelion, t P elC .q>

also the Arch A B will be less, and

{Ql &

quently the similar Arch e m, and jf st