Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data
We present an updated analysis of radial velocity data of the HD 82943 planetary system based on 10 yr of measurements obtained with the Keck telescope. Previous studies have shown that the HD 82943 system has two planets that are likely in 2:1 mean-motion resonance (MMR), with orbital periods about...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
| Published: |
American Astronomical Society
2013
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| _version_ | 1797097476485808128 |
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| author | Tan, X Payne, M Lee, M Ford, E Howard, A Johnson, J Marcy, G Wright, J |
| author_facet | Tan, X Payne, M Lee, M Ford, E Howard, A Johnson, J Marcy, G Wright, J |
| author_sort | Tan, X |
| collection | OXFORD |
| description | We present an updated analysis of radial velocity data of the HD 82943 planetary system based on 10 yr of measurements obtained with the Keck telescope. Previous studies have shown that the HD 82943 system has two planets that are likely in 2:1 mean-motion resonance (MMR), with orbital periods about 220 and 440 days. However, alternative fits that are qualitatively different have also been suggested, with two planets in a 1:1 resonance or three planets in a Laplace 4:2:1 resonance. Here we use χ2 minimization combined with a parameter grid search to investigate the orbital parameters and dynamical states of the qualitatively different types of fits, and we compare the results to those obtained with the differential evolution Markov chain Monte Carlo method. Our results support the coplanar 2:1 MMR configuration for the HD 82943 system, and show no evidence for either the 1:1 or three-planet Laplace resonance fits. The inclination of the system with respect to the sky plane is well constrained at $20^{+4.9}_{-5.5}$ degrees, and the system contains two planets with masses of about 4.78 M J and 4.80 M J (where M J is the mass of Jupiter) and orbital periods of about 219 and 442 days for the inner and outer planet, respectively. The best fit is dynamically stable with both eccentricity-type resonant angles θ1 and θ2 librating around 0°. |
| first_indexed | 2024-03-07T04:56:04Z |
| format | Journal article |
| id | oxford-uuid:d6a4ba3e-9445-4e9b-b9f7-4b13aa13ff55 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:56:04Z |
| publishDate | 2013 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | oxford-uuid:d6a4ba3e-9445-4e9b-b9f7-4b13aa13ff552022-03-27T08:35:01ZCharacterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity dataJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d6a4ba3e-9445-4e9b-b9f7-4b13aa13ff55Symplectic Elements at OxfordAmerican Astronomical Society2013Tan, XPayne, MLee, MFord, EHoward, AJohnson, JMarcy, GWright, JWe present an updated analysis of radial velocity data of the HD 82943 planetary system based on 10 yr of measurements obtained with the Keck telescope. Previous studies have shown that the HD 82943 system has two planets that are likely in 2:1 mean-motion resonance (MMR), with orbital periods about 220 and 440 days. However, alternative fits that are qualitatively different have also been suggested, with two planets in a 1:1 resonance or three planets in a Laplace 4:2:1 resonance. Here we use χ2 minimization combined with a parameter grid search to investigate the orbital parameters and dynamical states of the qualitatively different types of fits, and we compare the results to those obtained with the differential evolution Markov chain Monte Carlo method. Our results support the coplanar 2:1 MMR configuration for the HD 82943 system, and show no evidence for either the 1:1 or three-planet Laplace resonance fits. The inclination of the system with respect to the sky plane is well constrained at $20^{+4.9}_{-5.5}$ degrees, and the system contains two planets with masses of about 4.78 M J and 4.80 M J (where M J is the mass of Jupiter) and orbital periods of about 219 and 442 days for the inner and outer planet, respectively. The best fit is dynamically stable with both eccentricity-type resonant angles θ1 and θ2 librating around 0°. |
| spellingShingle | Tan, X Payne, M Lee, M Ford, E Howard, A Johnson, J Marcy, G Wright, J Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title | Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title_full | Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title_fullStr | Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title_full_unstemmed | Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title_short | Characterizing the orbital and dynamical state of the HD 82943 planetary system with keck radial velocity data |
| title_sort | characterizing the orbital and dynamical state of the hd 82943 planetary system with keck radial velocity data |
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