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Resonances and stability of extra-solar planetary systems

Published online by Cambridge University Press:  28 February 2005

C. Beaugé ,
N. Callegari ,
S. Ferraz-Mello  and
T.A. Michtchenko
C. Beaugé
Affiliation:
Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, (X5000BGR) Córdoba, Argentina (beaugé@oac.uncor.edu)
N. Callegari
Affiliation:
Departamento de Matemática, Universidade Federal de São Carlos, São Carlos, Brasil
S. Ferraz-Mello
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Cidade Univesitária, 05508-900 São Paulo, Brasil ([email protected])
T.A. Michtchenko
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Cidade Univesitária, 05508-900 São Paulo, Brasil ([email protected])
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Abstract

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This paper reviews recent results on the dynamics of multiple-planet extra-solar systems, including main sequence stars and the pulsar PSR B1257+12 and, comparatively, our own Solar System. Taking into account the degree of gravitational interaction of the planets, the known planetary systems may be separated into four main groups: (Ia) Planets in Mean-motion resonance (Ib) Low-eccentricity near-resonant pairs; (II) Non-resonant planets with a significant secular dynamics; and (III) Weakly interacting planet pairs. Different analytical and numerical tools can help to understand the structure of the phase space, to identify stability mechanisms and to categorize different types of motions in the cases of more significant dynamical interaction. The origin of resonant configurations is discussed in the light of the hypothesis of planetary migration.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Exoplanetsstabilityresonances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUC197 , August 2004 , pp. 3 - 18
Copyright
© 2005 International Astronomical Union