[ 2 45 ] 
another at equal intervals of time ; but differ fome- 
times by no lefs than 14, 15, or 16 hours j and there- 
fore, in order to know the true times of the returns 
of any eclipfe, recourfe muft be had to long and te- 
dious calculations. 
In order to fhew both the mean and true times of 
the above mentioned eclipfe, through all its periods, 
whilft it is vifible on this earth, together with the 
mean anomalies of the Sun and Moon, the true dis- 
tance of each conjunction from the afcending node, 
with the true latitude of the Moon at the time of each 
of her true conjunctions with the Sun, according to 
the old Stile, I have calculated the four following ta- 
bles, of which I beg the Royal Society’s acceptance. 
According to the mean (or fuppofed equable) mo- 
tions of the Sun, Moon, and nodes, the moon’s iha- 
dow in this eclipfe would have firffc touched the earth 
at the north pole, on the 13th of June, A.D. 1295; 
and would quite leave the earth at the fouth pole, on 
the 12th of September, A.D. 2665, at the com- 
pletion of its 77th period ; as fhewn in the firffc and 
fcond tables. 
But, on account of the true (or unequable) motions 
of the Sun, Moon, and nodes, the true lines of con- 
junctions of the Sun and Moon, and the Sun’s true 
diftance from the Moon’s alcending node, are as fet 
down in the third and fourth tables : and the Moon’s 
true latitude is too great at the end of the firft mean 
period, to allow her fhadow to touch the earth. So 
that the firft time of the coming-in of this eclipfe 
was at the end of its fecond mean period ; and the 
true time was on the 24th of June, A.D. 1313, 
at 
