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A Collisional and Self-Gravitational Model to Simulate Numerically the Dynamics of Planetary Disks

Published online by Cambridge University Press:  07 August 2017

Filomena Pereira Gama ,
Jean-Marc Petit  and
Hans Scholl
Filomena Pereira Gama
Affiliation:
Observatoire de la Côte d'Azur B. P. 139 06003 Nice Cedex FRANCE
Jean-Marc Petit
Affiliation:
Observatoire de la Côte d'Azur B. P. 139 06003 Nice Cedex FRANCE
Hans Scholl
Affiliation:
Observatoire de la Côte d'Azur B. P. 139 06003 Nice Cedex FRANCE

Abstract

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The dynamical evolution of the planetary rings is simulated by means of a numerical model in which particles interact through mutual attraction and inelastic collisions. We use a mixed simulation: a deterministic integration of the N - body problem for large distances (“particle-mesh” method with an expansion of density and potential in spherical harmonics) and a Monte Carlo treatment for the close encounters. The implementation is done in the Connection Machine in order to be able to make a detailed simulation using a greater number of particles (of the order of 105). The deterministic calculation of the action of a shepherding satellite on the particles will allow us to study the effect of resonances on the formation and the evolution of the sharp edges of the rings.

Keywords

planetary rings“particle-mesh” methodn-body simulationMonte Carlo methodconnection machine
Type
Part II - Planetary Rings
Information
Symposium - International Astronomical Union , Volume 152: Chaos, Resonance and Collective Dynamical Phenomena in the Solar System , 1992 , pp. 109 - 114
Copyright
Copyright © Kluwer 1992 

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