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Modelling the Evolution of Planets in Disks

Published online by Cambridge University Press:  20 January 2011

H. Wozniak ,
G. Hensler  and
W. Kley
W. Kley*
Affiliation:
Institute of Astronomy & Astrophysics, University of Tübingen, Germany
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Abstract

To explain important properties of extrasolar planetary systems (e.g. close-in hot Jupiters, resonant planets) an evolutionary scenario which allows for radial migration of planets in disks is required. During their formation protoplanets undergo a phase in which they are embedded in the disk and interact gravitationally with it. This planet-disk interaction results in torques (through gravitational forces) acting on the planet that will change its angular momentum and result in a radial migration of the planet through the disk. To determine the outcome of this very important process for planet formation, dedicated high resolution numerical modeling is required. This contribution focusses on some important aspects of the numerical approach that we found essential for obtaining successful results. We specifically mention the treatment of Coriolis forces, Cartesian grids, and the FARGO method.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 44: JENAM 2008: Grand Challenges in Computational Astrophysics , 2010 , pp. 107 - 116
Copyright
© EAS, EDP Sciences 2011

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