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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 

References

1. Sicardy, B. (1991) ‘Numerical experiment of perturbed collisional disks’, J. Comp. Phys. (to be published).Google Scholar
2. Lukkari, J. and Salo, H. (1984) ‘Numerical simulations of collisions in self-gravitating systems’, Moon and Planets 31, 1-.CrossRefGoogle Scholar
3. Hénon, M. and Petit, J.-M. (1986) ‘Series expansions for encounter-type solutions of Hill's problem’, Cel. Mechanics 38, 67–100.Google Scholar
4. Petit, J.-M. and Hénon, M. (1986) ‘Satellite encounters’, Icarus 66, 536–555.CrossRefGoogle Scholar
5. Petit, J.-M. and Hénon, M. (1987) ‘A numerical simulation of planetary rings. I. Binary encounters’, Astron. Astrophys. 173, 389–404.Google Scholar
6. Petit, J.-M. and Hénon, M. (1987) ‘A numerical simulation of planetary rings. II. Monte Carlo model’, Astron. Astrophys. 188,198–291205.Google Scholar
7. Gradshteyn, I.S. and Ryzhik, I.M. (1980) ‘Table of Integrals, Series and Products’, Academic Press, New York.Google Scholar
8. ‘A Poisson solver for ellipsoidal stellar systems’, private communication.Google Scholar
9. Morse, P.M. and Feshbach, H. (1985) ‘Methods of Theore tical Physics’, McGraw-Hill, New York.Google Scholar
10. Pereira Gama, F. and Petit, J.-M. (1990) ‘Statistical analysis of the effects of close encounters of particles in planetary rings’, Roy, A. E. (ed.), ‘Predictability, Stability and Chaos in N-Body Dynamical Systems’, Plenum Publishing Corporation (to be published).Google Scholar