DAVIES, Melvyn B.; ADAMS, Fred C.; ARMITAGE, Philip; CHAMBERS, John; FORD, Eric; MORBIDELLI, Alessandro; RAYMOND, Sean N.; VERAS, Dimitri

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DAVIES, Melvyn B.
Lund Observatory

ADAMS, Fred C.

ARMITAGE, Philip

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Communication dans un congrès

Ce document a été publié dans

Protostars and Planets VI, Henrik Beuther, Ralf S. Klessen, Cornelis P. Dullemond, and Thomas Henning (eds.), University of Arizona Press, Tucson, 914 pp., p.787-808, 2013-07-15, Heidelberg. 2014p. 787-808

Résumé en anglais

This chapter concerns the long-term dynamical evolution of planetary systems from both theoretical and observational perspectives. We begin by discussing the planet-planet interactions that take place within our own Solar System. We then describe such interactions in more tightly-packed planetary systems. As planet-planet interactions build up, some systems become dynamically unstable, leading to strong encounters and ultimately either ejections or collisions of planets. After discussing the basic physical processes involved, we consider how these interactions apply to extrasolar planetary systems and explore the constraints provided by observed systems. The presence of a residual planetesimal disc can lead to planetary migration and hence cause instabilities induced by resonance crossing; however, such discs can also stabilise planetary systems. The crowded birth environment of a planetary system can have a significant impact: close encounters and binary companions can act to destabilise systems, or sculpt their properties. In the case of binaries, the Kozai mechanism can place planets on extremely eccentric orbits which may later circularise to produce hot Jupiters.< Réduire

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804