[ ^44 J 
the fame eclipfe will have returned 38 times j and as 
the conjunction will then be only 24/ 45 ' ' from the 
node, the center of the Moon’s diadow will fall but 
a little northward of the center of the earth’s en- 
lightened difc. At the end of the next following 
period, the conjunction of the Sun and Moon will 
have receded back 3' 2 7" from the Moon’s amend- 
ing node, into the fouthern part of her orbit; which 
will caufe the center of her fhadow to pafs a very 
fmall matter fouth of the center of the earth’s difc. 
After which, in every following period, the conjunc- 
tion of the Sun and Moon will fall 28' 12" farther 
and farther back from the node, and the Moon’s 
fhadow will go dill further and further fouthward on 
the earth, until A. D. 2665, September 12, old 
ftile, at 23 11 46' 22" p.m, when the eclipfe will have 
finidied its 77th period, and will finally leave the 
earth at the fouth pole ; and cannot begin the fame 
courfe over the earth again in lefs than 12,492 years, 
as above mentioned. 
And thus, if the motions of the Sun and Moon 
were equable, the fame eclipfe would always return 
in 18 Julian years 1 1 days 7 hours 43 minutes 20 fe- 
conds, when the lad day of February in leap years 
is four times included in the period : but when it is 
five times included, the period is one day lefs ; or 1 8 
years 10 days 7 hours 43 minutes 20 feconds. 
But, on account of the various anomalies of the 
Sun and Moon, arifing from their moving in ecliptic 
orbs, and the effeCts of the Sun’s different attractions 
of the Moon in diderent parts of her orbit, the con- 
junctions of the Sun and Moon never fucceed one 
5 another 
