Equilibrium theory for Saturn's ring with self-gravitation and finite thickness

Details Equilibrium theory for Saturn's ring with self-gravitation and finite thickness Equilibrium theory for Saturn's ring with self-gravitation and finite thickness

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...138..290s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 290-296. Research supported by the Deutsche Forschu

Astronomy and Astrophysics

Astrophysics

3

Equilibrium Equations, Planetary Evolution, Planetary Gravitation, Saturn Rings, Density Wave Model, Poisson Equation, Stellar Motions, Thickness, Saturn, Rings, Equilibrium, Hypotheses, Gravity Effects, Thickness, Pressure, Isotropy, Velocity, Models, Evolution, Distribution, Particles, Orbits, Radial Distance, Structure, Features, Parameters, Oscillations, Density, Dynamics, Theoretical Studies

Scientific paper

In the present discussion of the equilibrium of Saturn's ring within the purview of kinetic theory, self-gravitation and the finite thickness of the ring are taken into account and pressure anisotropy in the velocity plane (perpendicular to the bulk velocity) is allowed for. This effort may further current work toward a quantitative theory of planetary ring evolution. A particle distribution function satisfying Boltzmann's equation in the collisionless limit is chosen which is appropriate for thin rings, and a corresponding fluid approach is used. For typical values of the relevant physical parameters, self-gravitation effects are expected to be small, but not negligible. Two explicit equilibrium examples are given.

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