of the Georgian planet. 
35 1 
Explanation of the identifying method. 
It is evident, that we cannot be satisfied with a conclusion 
that is drawn from the apparent situation of an observed 
satellite, if a doubt should remain whether it actually was the 
satellite which it is said to be; and where such numerous 
observations are to be examined, a method of identifying tl\e 
satellites becomes absolutely necessary. 
When the periodical revolution is known, the place where 
a satellite at any given time should be seen, may be strictly 
calculated ; but a method somewhat less rigorous, and much 
more expedient, will be sufficient for the purpose ; but even 
this will be found to require tedious computations ; for in the 
firs place, the motion of the satellite to be identified for any 
day, must be cast up by the table of its motion in days, hours, 
and minutes; and for this purpose, the interval of time for 
which it is calculated, must first be ascertained ; this has been 
done f r every day the satellites have been observed. The 
amoi . of the motion in orbit being obtained, it must be added 
to th mber of degrees from which the motion proceeded ; 
this ■ the already mentioned general epoch of 1787, Feb. 16, 
9 0 38' was for the first satellite 11 0 27' from the node, and 
for the econd 5 0 6'. The sum then will be the real place 
of the satellite in its orbit. 
Now, to obtain the apparent place of a satellite from a given 
real one, a table must be made, the first column of which 
must contain the degree of the geocentric longitude of the 
plane r which the rest of the columns are calculated. The 
three analogies that have been given, are to be used for ob- 
taining the contents of the second, third, and fourth columns; 
