[ 449 3 
the moon’s parallax of latitude in eclipfes ; but this be- 
ing deduced or added as the cafe requires gives EH, 
which being augmented in the proportion of the fine of 
BD-|-DC to the fine of BD, gives truly the apparent 
latitude without fenfible error, when the latitude is 
fmall : But, when greater, requires to be corredled by 
adding together the logarithmic fine of the latitude now 
found, the fine of EH and the logarithm of DE, 
tht fum of which is the double of the corred:ion re- 
quired. 
In the laft place the moon’s horizontal . diameter 
augmented in the proportion of the fine of BC to 
the fine of BD exhibits the moon’s apaprent diameter. 
And here the calculation will proceed thus : 
In the example above chofen for computing the 
nonagefime degree. 
The moon’s longitude is given from T 6l*. 2/38" 
The longitude of the nonagefime 
degree was found above to be 
Therefore BD = 7. 6. 14^ 
~ -its fincj 
BZ, as found above, 50°. 2'. 0''. its cofine 
The horizontal parallax in feconds 
9.09226 
9.80777 
3-52387 
» ■ O / // 
4.25 
This added to BD gives 7. 10. 39 
Its fine 
2.42390 
9.09673 
Diff. from the firft fine 
This added to the log. of 4'. 25", gives the* 
log. of 4'. 28", for the moon’s parallax in lon- 
gitude, fuch.as is derived from the parallax in 
altitude by the parallactic angle, , J 
447 
2.42837 
VoL. LXI. 
M m m 
Again, 
