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Formation, migration, and stability of extrasolar planetary systems
Adams, Fred C.
Dynamics of Populations of Planetary Systems, Proceedings of IAU Colloquium #197, held 31 August - 4 Spetember, 2004 in Belgrade, Serbia and Montenegro. Edited by Z. Knezevic and A. Milani. Cambridge: Cambridge University Press, p.19-28
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Extrasolar planets, planetary dynamics, planet formation.
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This paper presents recent results concerning the planet formation, planet migration, and the long term stability of planetary systems. Most stars are found in binary systems and binary companions can disrupt both planet formation and stability. We first consider the effects of outer binary companions on the late stages of terrestrial planet formation and show how planet formation depends on the binary periastron. We then consider migration mechanisms for giant planets. In this case, planet scattering produces the full range of orbital eccentricities, but is less effective in moving planets inward (decreasing their semi-major axes). Disk torques are effective at moving planets inward, but not at increasing the eccentricities. We explore a scenario in which disk torques act in concert with planet scattering to provide the full range of orbital elements observed in extrasolar planetary systems. Finally, we consider the longer term stability of Earth-like planets in binary systems; we find that nearly 50 percent of binaries allow for Earth-like planets to remain stable over the current (4.6 Gyr) age of our solar system.

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