2 35

to L e c t u r e XL

not Lmg to make it otherwise) it sol-V e( j *^ a t the Times (i. e. the Days) mea-v the Sun in the Ecliptic must be al-tiofa ^cqual; or, in other Words,

the

~' a ys are sometimes shorter, sometimesu 8er.

th,

than the equal Time measured out<( j 6 ^fiuinoctial.

^ T has been shewn already, that thepotion of the Earth precedes theN j s 111 the first Semicircle of Anomaly,\j.^P rece ded by the Mean in the second,. ° re while the Earth is going from^ Phelion to the Perihelion, or whileapparently moves from the Apo-Ml} ^ to the Perigæum, the Apparent Time'Vrj ,C before the Mean, and in the other^ of Anomaly it will be after it.\ ^ erence of these Motions convertedIW l hte is the Equation of Time in thisa nd is to be subtracted from the Ap-

° ts e / lrtle to gain the Mean, or addedr sl ^ ^an to gain the Apparent, in the

lr> tsp^^hcle of Anomaly, and vice versa2 atter.

S 9 ; f N °W both these Parts of the Equa-r. ^tme' are calculated by Astrono-w ° r every Degree of Anomaly, and

fr

o r

ev

' l 'e p C . r .y Degree of the Sun’s Longitude in"Die, and disposed in two several

Tables,