Orbital stability constraints on the nature of planetary systems
Abstract
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.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- December 1981
- DOI:
- 10.1086/159468
- Bibcode:
- 1981ApJ...251..337G
- Keywords:
-
- 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;
- Astrophysics