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Dynamics of Circumstellar Planets in Binary Star Systems

Published online by Cambridge University Press:  16 October 2024

Man Hoi Lee Open the ORCID record for Man Hoi Lee [Opens in a new window] ,
Ka Ho Wong ,
Ho Wan Cheng Open the ORCID record for Ho Wan Cheng [Opens in a new window] ,
Trifon Trifonov ,
Sabine Reffert  and
Andreas Quirrenbach
Man Hoi Lee*
Affiliation:
Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong
Ka Ho Wong
Affiliation:
Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong
Ho Wan Cheng
Affiliation:
Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong
Trifon Trifonov
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
Sabine Reffert
Affiliation:
Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
Andreas Quirrenbach
Affiliation:
Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
*
email: [email protected]
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Abstract

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Circumstellar planets in binary star systems provide unique constraints on the formation and dynamical evolution of planets. We present an empirical formula for the stability boundary of coplanar retrograde orbits, similar to the classic one for coplanar prograde orbits. We discuss two of the tightest binaries with circumstellar planets: HD 59686 and ν Octantis. For HD 59686, dynamical fitting of the radial velocity data and stability analysis show that the planet must be either on a nearly coplanar retrograde orbit or in one of the narrow regions of prograde orbits stabilized by secular apsidal alignment. For ν Octantis, a nearly coplanar retrograde planetary orbit is the only option for dynamical stability. We also discuss the mysterious case of ε Cygni. It shows short-period radial velocity variations that closely resemble the signal of a Jupiter-mass planet, but the period and amplitude change over time and dynamical stability analysis rules out a planet.

Keywords

planetsbinary starsstabilityHD59686ν Octantis
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S382: Complex Planetary Systems II: Latest Methods for an Interdisciplinary Approach , December 2022 , pp. 12 - 19
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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