Satellites of the Georgium Sidus , &c. 65 
when a smaller one very near it was scrupulously recorded. 
The motion of the planet, in 3 hours and 3 minutes, is men- 
tioned as very visible. The place of the star, which was a new 
visitor this evening, was very particularly delineated, at 6 h 50'. 
From its situation, it is evident the motion of the planet must 
have carried this star, if it was one of its satellites, towards the 
large star f figure 3 ; in the light of which a dim satellite 
would be lost. This accordingly happened ; for at io h 7' and 
io h 21/ it was no longer visible. The direction of the planet's 
motion is plainly pointed out, by the place of the planet 
March 2d. 
With respect to the orbit of this satellite, it appears, from its 
situation near the apogee, where it was seen, that its distance 
was to that of the second satellite, which was then near its 
greatest elongation, as 8 to 5. And, since the apogee distance, 
on the day of observation, was only ,37, we have its greatest 
elongation as — to 5; that is, as 21,6 to 5, or above 4 to 1. 
From which we may conclude, that its orbit must lie consi- 
derably without the before mentioned exterior satellite of Feb. 
9 > ! 79 0 - 
We have a second observation of it March 27, 1794 ; which, 
though not very strong, yet adds confirmation to the former. 
For that evening, which was uncommonly fine, other satellites, 
south, at a good distance, were perceived. This must relate 
principally to our present satellite, which may certainly be said 
to be at a good distance from the planet, and which, by that 
time, was probably in the southern part of its orbit, and near 
its greatest elongation. 
There is a third observation, March 28, 1797, which probably 
also belongs to this satellite. For the exceedingly small star Y, 
mdccxcviil • K 
