[ +*4 ] 
V aa — uuy when we fuppofe, after the integration. 
rr 
- — u ; and 
r 
aa Ctt ^ a& a a ir 
~x ~~~ % ~ X — — — . 
rr 2.r rr 4 r r 
Therefore 
the preceflion from the fun’s departure from the equi- 
nox till his arrival at the folftice, is A b x ?"x — — x 
2 4 rr 
( 1 — A b x — x-j" ) = ( g being = — ) A b x 
27rg rrS 0 0 
^ x - x ( I — £ x x 4). 
27rr 
When the motion of the node is not very fenfible, 
it will fuffice to make ufe of the formula of the pre- 
ceding Problem , which is the firft term of this ; But 
when that motion is fenfible, which is the cafe of the 
moon's node, when it is to be determined for a quar- 
ter of the revolution of the fun, it will be requifite 
to employ this formula ^ which contains two terms of 
the feries. Nay, it would be very eafy to take a greater 
number of terms, fo as to negledl nothing; but this 
would be abfolutely ufelcfs, becaufe of the quick con- 
verging of the feries. 
Pro- 
