6o Dr. Herschei/s Discovery of Jour additional 
the satellite's coming to the apogee, it might easily happen that 
the least change in the clearness of the air, during a time of 
i h 5', which elapsed between the first and second observation, 
might render an object invisible, which, as the first observa- 
tion says, was “ excessively faint, and could only be seen by 
glimpses." 
From the observed distance, which is put at “ 2 diameters 
of the planet," we may conclude what would be the distance 
of its greatest elongation. For, 2 diameters from the disk of 
the planet give 2-§- from the centre. Now, the distance of the 
apogee at this time, by my tables, was ,64, supposing that of 
the greatest elongation 1 ; therefore we have the radius of its • 
u 
<< 
orbit 
2,5 X 4",I2 
,64 
i6",i. 
This calculation is not intended to determine precisely the 
distance of the satellite, but only to shew that its orbit is more 
contracted than that of the 1st, and that consequently it is an 
interior satellite. 
If any doubt should be entertained about the validity of this 
observation, we have a second, and very striking one, of March 
5, 1794; where an interior satellite was suspected south fol- 
lowing the planet, at one-third of the distance of the 1st. 
March 4, when a description was made of the stars, as in 
figure 4, this satellite was not in the place where it was ob- 
served the 5th. And, by an examination of the same stars 
March 7, it appears, that even the smallest stars n m 0, of the 
5th, were seen in their former places, but not the satellite. 
The observation therefore must be looked upon as decisive with 
regard to its existence. If any doubt should arise, on account 
of the suspicion not being verified with 480, I must remark, 
that being used to such imperfect glimpses, it has generally 
