The lynx. (Panola, Mi. [i.e. Miss.]) 1845-1845, 1845-09-13

compllshmentsol several important MAJ
ters connected with these wonderful
objects. 1t has already been seen that
tire conditions Of equilibrium ofSaturn's
rings. require that these rings should
be OF an equal thickness or Of on equal
density. The period of the disappear
ance Of the rings has been successful
ly used by Bessel, for the purpose of
procuring data TO determine The follow
ne points:
LIST. The notice Of The surfaces Of the
rings, whether plane or curved.
Cd. The inclination OF the mean
plane ofthe rings to The ccliptic.
Sd. The parallelism of the two surfa.
ces which bound the rings on opposite
sides.
All the observations from the year
1901 TO 1852, inclusive, have been
collected and fully discussed. At the
disappearance of the ring in 1901, it
seems that the western handle was Wis
IDLE longer than the eastern.
The same popularity was exhibited
in l7f4, and in 1915, the western ansa
was the last 10 fade from the sight and
the first 10 re-appear. In 1774, at
the second Ie-appearance of the ring,
Messier first observed the eastern han
die or ansa, on the morning Of the list
July. At the first temperance in
1888, Micbain first saw very faint
return of the eastern handle; at the
second re- appearance, the same ansa,
first became visible. In the year g.
OF, the eastern haqdle remained long
est visible, while at The temperance,
Harding Of Lilienthal. first remarked
the returning light on the western han
Gle. Now in case the rings Of Saturn
were bounded on either side by a par
aliel plane surfaces, it is difficult TO con-
ceFe any reason why one handle should
not fade from the sight at precisely the
time instant with the other.
While on the contrary an unequal
thickness in some parts OF the ring
would present broader surGace on the
1, edge IN some nlaSns than in others and
thus account for The phenomenon as
recorded.
As the rings shine by the reflected
light Of the sun, in case the broad fiat
surface is in any degree uhduaiing.
the elevation ought TO cast long and
dark shadows, at the time that the
plane Of the ring comes nearly TO spass
through the sun. S5'lar as observation
goes, no trace Of such shadows have as
yet been discovered. This would seem
TO indicate great eveness in the gen
eral surface, and taken in connection
with tie preceding facts, would lead
us to he conclusion that the rings are
actually thicker in some places than in
others. Admit such unequal thickness
and the rotation of-the rings on an ak
is perpendicular to their plane, and all
the phenonehons recorded at the mp
pearance and disappea rance ofthe fings
are easily accounted for.
At the time the rings disappear in
ordinary telescopes, they may still be
seen in the very largest and best in
struments as fine line of light, pass
ing directly through the centre of the
planet. This most interesting pheuom-
enon will probably be seen for the first
time in the New World in the year
| 1947. AL the last disappearance ia 49,
| SO, '33, Hetshel was able TO discern
the edge of the rings resembling d fire
thread of light, upon which he de
scribes the satellites strung like beads
Owingto the inclination under which
the rings of Saturn are always seen,
it will never be possible TO ascertain
their figure in any other way than by
| computation. NO measurements nave
vel been made Of sufficient delicacy to
detect any eccentricity III the figure oil
the rings.
They appear 10 be exactly circular
at}d indeed the orbits Of the two inner
satellites have not been discovered TO
differ from the same figure That
these rings exert powerful influence
on the planes of the orbits of the near
err satellites must be evident, from the
fact that all the nearer satellites revolve
in orbits where planes are nearly com
idcent with that oflhe ring. Indeed Sir
William Herschel was disposed to at
tribute TO the influence of the rings, a
remarkable appearance which ne an