274 PHILOSOPHICAL TRANSACTIONS. [ANNO 1798. 



very small star was seen, in a place where the evening before there had been none ; 

 as appears by the configuration of the 5th of March. At the time of the obser- 

 vation, the planet was come to the longitude of the place where the star was per- 

 ceived to be ; which agrees with the idea of its having been brought to that situ- 

 ation by the planet. It may be objected, that the star could not be verified with 

 a power of 600 ; but here we have more than a bare suspicion of the satellite, for 

 the observation says, I had a pretty certain glimpse of it ; and this appears also 

 from the assigned place of the star at the intersection of 2 given lines. For, such 

 a delineation could not have been made, without having perceived it with a consi- 

 derable degree of steady vision. Its distance, to judge by the description, will agree 

 sufficiently with the foregoing 2 observations of this exterior satellite. 



The most distant satellite. — On Feb. 28, 1794, a star was perceived where on 

 the 26th there was none. This star was larger than a very small star which was 

 observed the 26th, not far from the place of the new supposed satellite ; and a 

 configuration having been made expressly, by way of ascertaining what stars might 

 afterwards come into a situation where they could be mistaken for satellites, our 

 new star or satellite would not have been omitted, when a smaller one very near it 

 was scrupulously recorded. The motion of the planet in 3 h 3 m , is mentioned as 

 very visible. The place of the star, which was a new visitor this evening, was very 

 particularly delineated, at 6 h 50 m . From its situation, it is evident that the motion 

 of the planet must have carried this star, if it was one of its satellites, towards a 

 large star near it ; in the light of which a dim satellite would be lost. This ac- 

 cordingly happened ; for at 10 h 7 m and 10 h 21 m it was no longer visible. The di- 

 rection 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 2d satellite, 

 which was then near its greatest elongation, as 8 to 5. And since the apogee dis- 

 tance, 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 con- 

 clude, that its orbit must lie considerably without the before-mentioned exterior 

 satellite of Feb. 9, 179°- 



We have a 2d 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 3d observation, 

 March 28, 1797, which probably also belongs to this satellite. For an exceed- 

 ingly small near star, which is mentioned as not having been seen the 25th, when 

 the delineation of the stars was made, will agree very well with the 2 former ob- 

 servations ; and, being near the greatest elongation, the distance of this satellite 



