Two giant planets orbiting the K giant star η Cet
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 plane...
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| Other Authors: | , , |
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| Format: | Article (Journal) Conference Paper |
| Language: | English |
| Published: |
2013
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| In: |
Proceedings of the International Astronomical Union
Year: 2013, Volume: 8, Issue: S299, Pages: 309-310 |
| ISSN: | 1743-9221 |
| DOI: | 10.1017/S1743921313008739 |
| Subjects: | |
| Online Access: | Verlag, Pay-per-use, Volltext: http://dx.doi.org/10.1017/S1743921313008739
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| Author Notes: | T. Trifonov; S. Reffert; X. Tan; M. H. Lee; A. Quirrenbach |
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| 520 | |a 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. | ||
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