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Two Giant Planets Orbiting the K Giant Star η Cet

Published online by Cambridge University Press:  06 January 2014

T. Trifonov ,
S. Reffert ,
X. Tan ,
M. H. Lee  and
A. Quirrenbach
T. Trifonov
Affiliation:
ZAH-Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
S. Reffert
Affiliation:
ZAH-Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
X. Tan
Affiliation:
Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong
M. H. Lee
Affiliation:
Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong
A. Quirrenbach
Affiliation:
ZAH-Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
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Abstract

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We present evidence of a new planetary system around the K giant η Cet (HIP 5364, HD 6805, HR 334), based on 124 high-precision optical and infrared radial velocity data, taken at Lick Observatory (Hamilton) and at VLT (CRIRES). The best dynamical fit to the data is consistent with two massive planets (m1sini≈2.6MJup, m2sini≈3.3MJup) and with periods of P1≈407 days, P2≈740 days. To test the η Cet system's stability we perform ~ 10,000 dynamical investigations with maximum time spans of 108 years. We find that in case of moderate eccentricities, the planets can be effectively trapped in an anti-aligned stable 2:1 mean motion resonance (MMR), very close to the separatrix. A larger non-resonant stable region exists in low-eccentricity parameter space, although less probable than the 2:1 MMR region.

Keywords

techniques: radial velocitiesmethods: numericalplanetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 309 - 310
Copyright
Copyright © International Astronomical Union 2013 

References

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Lee, M. H. 2004, ApJ, 611, 517LCrossRefGoogle Scholar