C 74 ] 
=.9001387: whence the whole motion, found as 
above directed, will be 10962" = 3* 2' 42 ' ; the 
correction, on account of the excentricity, being 
only 2 1 7 . 
Multiply 3 0 2' 42' by 1.08085-3, and the pro- 
duct 3° 17' 28" is the mean motion of the apogee, 
in a fynodical month ; exceeding the quantity marked 
in the tables by no more than 4". 
1 7. Of the obliquity of the moon’s orbit, to the plane 
of the ecliptic, we take no notice : becaule, altho’, 
abfolutely fpeaking, a force in that plane, referred to 
the moon’s orbit, would, thence, be diminifhd by 
about ~o 6 ~ P^ts j yet, in the prefen t cafe, the effeCt 
of the obliquity is included in the firft determination 
of the quantity c, from the periodical times of the 
earth and moon 3 all but what belongs to the cor- 
rections 3 and which is only 1 io^.xoo^ o' 7 . 2 2, to be 
fubtraCted. 
18. The force c is, itfelf, the effeCt of the fun’s 
parallax, and the total effeCt 3 excepting only a fmall 
difference between his aCtion on the moon, when fhe 
is waxing or waning, and when fhe is in the other 
half of her orbit 3 negledtcd as altogether inconfider- 
able. 
Upon the whole, we may conclude, that, in this, 
as in the other phenomena of the celeflial motions, 
the principles and rules of Sir Ilaac Newton are fully 
confirmed and verified, 
XII. 
