Orbital stability constraints on the nature of planetary systems

Details Orbital stability constraints on the nature of planetary systems Orbital stability constraints on the nature of planetary systems

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251..337g&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 1, 1981, p. 337-341.

Astronomy and Astrophysics

Astrophysics

48

Gas Giant Planets, Motion Stability, Orbital Mechanics, Planetary Systems, Protoplanets, Solar Orbits, Stellar Gravitation, Computerized Simulation, Constraints, Gravitational Effects, Many Body Problem, Secular Variations, Self Consistent Fields, Solar System

Scientific paper

A fully self-consistent, N-body computer code is used to study conditions under which model planetary systems, each consisting of a star and two 'planetary' companions, become orbitally unstable as a result of gravitational interactions between the companions. A formula describing a necessary condition for orbital stability is given. It is found that giant gaseous protoplanets of the type postulated by Cameron (1978) to be precursors of the present-day solar system planets could have stable orbits for at least 10,000 years, the time required for significant core formation in a typical giant gaseous protoplanet.

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