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Orbital stability of planets in binary systems: A new look at old results

Published online by Cambridge University Press:  01 October 2007

J. Eberle ,
M. Cuntz  and
Z. E. Musielak
J. Eberle
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019-0059, USA email: cuntz@uta.edu, zmusielak@uta.edu
M. Cuntz
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019-0059, USA email: cuntz@uta.edu, zmusielak@uta.edu
Z. E. Musielak
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019-0059, USA email: cuntz@uta.edu, zmusielak@uta.edu
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Abstract

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About half of all known stellar systems with Sun-like stars consist of two or more stars, significantly affecting the orbital stability of any planet in these systems. This observational evidence has prompted a large array of theoretical research, including the derivation of mathematically stringent criteria for the orbital stability of planets in stellar binary systems, valid for the “coplanar circular restricted three-body problem”. In the following, we use these criteria to explore the validity of results from previous theoretical studies.

Keywords

Astrobiologymethods: numericalbinariesplanetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 507 - 510
Copyright
Copyright © International Astronomical Union 2008

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