130 
DR. G. R. GOLDSBROUGH ON THE INFLUENCE OF SATELLITES, ETC. 
Satellite Rhea should also produce a clearance of particles up to radius 13 "07". 
The inner edge of Ring B is observed to commence at 13 "21". 
The existence of the Crepe Ring in a dissipative area is also discussed. 
(4) By the inclusion of the effect of the oblateness of Saturn and the influence of 
one ring of particles upon another these results might be still further improved. 
The theory presented therefore gives a closely quantitative account of the salient 
features of Saturn’s Ring. The numerous smaller divisions observed by Lowell and 
others are not accounted for ; but, for the reasons given in § 4, their existence is not 
excluded. 
(5) The dimensions of Cassini’s Division show that particles of all sizes up to a 
limit just short of that imposed by Maxwell for stability exist in the rings. 
Appendix on the Data of the Problem. 
I. Dimensions and divisions of the ring in seconds of arc at mean distance^ :— 
Distance from centre of planet to— 
Inner edge of Crepe Ring 
. 
. 10-83" 
Inner edge of Ring B 
O 0 
Bl 
. 
. 13-00" 
. 13-39" 
B2 
. 14-04" 
Divisions of Ring B -< 
B3 
B4 
. 14-74" 
. 15-32" 
B5 
. 15-69" 
-B6 
. 15-95" 
Outer edge of Ring B . 
C> O 
. 16'87" 
Inner edge of Ring A . 
. 17-64" 
Division in Ring A . 
. 
. 19‘00" 
Outer edge of Ring A . 
0 0 
. 20‘01" 
II. 
Equatorial diameter of Saturn . 
. 17-30" 
III. 
Elements of satellites :— 
Mean distance. 
Mass 
as fraction of Saturn. 
Mimas. 
26'82 // 
7 . 10- 8 
Enceladus. 
34M3" 
25.10- 8 
Tethys . . . . 
. 
42-66" 
11 . 10- 7 
Dione. 
54-59" 
18'7 . 10- 7 
Rhea 
76-38" 
4 . 10- 6 
Titan. 
174-8" 
2'1 . 10- 4 
* Lowell, ‘Observatory Bulletin,’No. 6S, and “Lecture” on April 26, 1916, in ‘Journal of Royal 
Astron. Soc. of Canada.’ 
rhLSLRTfiD 
2 G OCT. 1921 
