of the Georgian planet. 361 
must have been 72 0 np ; and its distance exceeded that of the 
second satellite. 
Addition. 
The 31st of January, 1791, a satellite in opposition to tne 
second, and at about double the distance from the planet was 
observed; its identified position was 78^ 0 np. The 2d of 
February all the stars of the configuration that had been 
pointed out, were seen remaining in their places, but the 
exterior satellite was not among them. 
The 26th of February, 1792, a star at double the distance 
of the first satellite was pointed out, but it has not been 
accounted for in succeeding observations. By remark IV, 
however, faint exterior satellites can hardly be' expected to 
be seen at any other time, than when they are about their 
greatest elongation. 
The 11th of February, 1798, an exterior satellite, called 
the fifth, was observed ; its situation was measured 89° 19', 5 
nf. The 13th of February, this satellite was no longer in the 
place where it had been seen the 11th. The 15th of February 
it w r as again ascertained that the satellite had left its former 
situation. The orbits of the satellites, at the time of these 
observations, were already contracted into a line, and a very 
faint satellite like this could not remain visible two, and four 
days successively ; its motion, according to remark IV, would 
in a short time immerge it again into the effusive light of the 
planet, and render it invisible. 
More distant satellites. 
The 28th of February, 1 794, a small star was seen in a 
place where the 26th there was none. By the configuration 
MDCCCXV. 3 A 
