on the Planet Saturn . 
*3 
except in very fine weather, it cannot eahly be feen well 
enough to take its place with accuracy. On the other hand, 
the greateft elongations allow fo much latitude for miftaking 
its true fituation, that it will require a confiderable time to 
divide the errors that muft arife from imperfedl eftimations. 
The orbits of tnefe two latellites, as appears from many 
obfervations of them, are exaftly in the plane of the ring, or 
at leaft deviate fo little from it, that the difference cannot be 
perceived. It is true, there is a poffibility that the line of 
their nodes may be in, or near, the prefent greateft elongation, 
in which cafe the orbits may have fome fmall inclination ; but 
as I have repeatedly feen them run along the very minute arms 
of the ring, even then the deviation cannot amount to more 
than perhaps one or two degrees; if, on the contrary, the 
nodes fhould be fituated near the coujundtion, this quantity 
would be fo confiderable that it could not have efcaped my 
obfervation. 
From the ring and Satellites of Saturn we now turn oui 
thoughts to the planet-, its belts, and its figure. 
April 9, * 775 * I obferved a northern belt on Saturn, which 
was a little inclined to the line of the ring. 
May 1, 1776. There was another belt, inclined about 15 de- 
grees to the fame line, but it was more to the 
louth, and on the following fide came up to the 
place in which the ring crofles the body. 
July I3> The belt was again depreffed towards the 
north, almoft touching the line where the ring 
paflfed behind the body. 
April 8, 1777. There were two fine belts, both a little in- 
clined to the ring. 
June 
