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Formation and Orbital Evolution of Planets

Published online by Cambridge University Press:  23 April 2012

Wilhelm Kley
Wilhelm Kley*
Affiliation:
Institut für Astronomie & Astrophysik, Universität Tübingen, Morgenstelle 10, 72076 Tübingen, Germany email: [email protected]
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Abstract

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The formation of planetary systems is a natural byproduct of the star formation process. Planets can form inside the protoplanetary disk by two alternative processes. Either through a sequence of sticking collisions, the so-called sequential accretion scenario, or via gravitational instability from an over-dense clump inside the protoplanetary disk. The first process is believed to have occurred in the solar system. The most important steps in this process will be outlined. The observed orbital properties of exoplanetary systems are distinctly different from our own Solar System. In particular, their small distance from the star, their high eccentricity and large mass point to the existence of a phase with strong mutual excitations. These are believed to be a result of early evolution of planets due to planet-disk interaction. The importance of this process in shaping the dynamical structure of planetary systems will be presented.

Keywords

planetary systems: formationaccretion diskshydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 429 - 436
Copyright
Copyright © International Astronomical Union 2012

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