Other
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...58..169s&link_type=abstract
(IAU, COSPAR, NASA, et al., Colliquium on Natural Satellites, 77th, Cornell University, Ithaca, NY, July 5-9, 1983) Icarus (ISSN
Other
9
Orbit Perturbation, Particle Motion, Planetary Orbits, Saturn Rings, Saturn Satellites, Astronomical Photography, Dynamic Models, Lagrangian Equilibrium Points, Orbital Velocity, Voyager 1 Spacecraft, Voyager 2 Spacecraft, Saturn, Rings, E Ring, Dynamics, Observations, Photographs, Brightness, Distance, Size, Width, Satellites, Particles, Motion, Analysis, Orbits, Librations, Lagrange Points, Voyager 1, Voyager 2
Scientific paper
Photographic evidence for a wide outer ring of Saturn, the E ring, was first introduced in 1967 and detailed observations were obtained in 1980. The brightness profile of the E ring indicates that the ring extends from three Saturn radii, the orbit of Mimas, to at least eight Saturn radii, just inside the orbit of Rhea. The brightness profile has a peak at the orbit of Enceladus, but to the limit of the observations there is no evidence of variations in the brightness profile at the orbital distances of Tethys or Dione. It is known that there are satellites at the Lagrangian points of Tethys and Dione within the E ring. Thus the E ring is not constrained by satellites, but rather coexists at the same orbital distances as satellites which have other satellites at their Lagrangian points. Preliminary numerical and analytical investigations of the motions of the particles indicate the majority of the particles are strictly influenced by Saturn. Particles in narrow rings at the orbital distance of a satellite move with revolution or librational motion and sometimes switch between these modes. The librational motion can be tadpole orbits at the L4 and L5 points, horseshoes including L4, L3, and L5 points and segment librations between the L4 or L5 points and the satellite.
Harrington Robert S.
Seidelmann Kenneth P.
Szebehely Vector
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