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Orbital stability of Earth-type planets in stellar binary systems

Published online by Cambridge University Press:  21 October 2010

Jason Eberle ,
Manfred Cuntz  and
Zdzislaw E. Musielak
Jason Eberle
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX, USA email: wjeberle@uta.edu, cuntz@uta.edu, zmusielak@uta.edu
Manfred Cuntz
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX, USA email: wjeberle@uta.edu, cuntz@uta.edu, zmusielak@uta.edu
Zdzislaw E. Musielak
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX, USA email: wjeberle@uta.edu, cuntz@uta.edu, zmusielak@uta.edu
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Abstract

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An important factor in estimating the likelihood of life elsewhere in the Universe is determining the stability of a planet's orbit. A significant fraction of stars like the Sun occur in binary systems which often has a considerable effect on the stability of any planets in such a system. In an effort to determine the stability of planets in binary star systems, we conducted a numerical simulation survey of several mass ratios and initial conditions. We then estimated the stability of the planetary orbit using a method that utilizes the hodograph to determine the effective eccentricity of the planetary orbit. We found that this method can serve as an orbital stability criterion for the planet.

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 691 - 692
Copyright
Copyright © International Astronomical Union 2010

References

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