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The formation of massive planets in binary star systems

Published online by Cambridge University Press:  19 April 2010

K. Goździewski ,
A. Niedzielski ,
J. Schneider  and
W. Kley
W. Kley*
Affiliation:
Institute of Astronomy & Astrophysics, University of Tübingen, Germany
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Abstract

As of today over 40 planetary systems have been discovered in binary star systems. In all cases the configuration appears to be circumstellar, where the planets orbit around one of the stars, the secondary acting as a perturber. The formation of planets in binary star systems is more difficult than around single stars due to the gravitational action of the companion on the dynamics of the protoplanetary disk. In this contribution we first briefly present the relevant observational evidence for planets in binary systems. Then the dynamical influence that a secondary companion has on a circumstellar disk will be analyzed through fully hydrodynamical simulations. We demonstrate that the disk becomes eccentric and shows a coherent precession around the primary star. Finally, fully hydrodynamical simulations of evolving protoplanets embedded in disks in binary star systems are presented. We investigate how the orbital evolution of protoplanetary embryos and their mass growth from cores to massive planets might be affected in this very dynamical environment. We consider, in particular, the planet orbiting the primary in the system γ Cephei.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 42: Extrasolar Planets in Multi-Body Systems: Theory and Observations , 2010 , pp. 227 - 238
Copyright
© EAS, EDP Sciences, 2010

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