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Article: Precise radial velocities of giant stars: XIII. A second Jupiter orbiting in 4:3 resonance in the 7 CMa system

TitlePrecise radial velocities of giant stars: XIII. A second Jupiter orbiting in 4:3 resonance in the 7 CMa system
Authors
Keywordstechniques: radial velocities
planetary systems
planets and satellites: dynamical evolution and stability
planets and satellites: detection
Issue Date2019
PublisherEDP Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy & Astrophysics, 2019, v. 631, p. A136:1-A136:8 How to Cite?
AbstractWe report the discovery of a second planet orbiting the K giant star 7 CMa based on 166 high-precision radial velocities obtained with Lick, HARPS, UCLES, and SONG. The periodogram analysis reveals two periodic signals of approximately 745 and 980 d, associated with planetary companions. A double-Keplerian orbital fit of the data reveals two Jupiter-like planets with minimum masses mb sini ~ 1.9 MJ and mc sini ~ 0.9 MJ, orbiting at semimajor axes of ab ~ 1.75 au and ac ~ 2.15 au, respectively. Given the small orbital separation and the large minimum masses of the planets, close encounters may occur within the time baseline of the observations; thus, a more accurate N-body dynamical modeling of the available data is performed. The dynamical best-fit solution leads to collision of the planets and we explore the long-term stable configuration of the system in a Bayesian framework, confirming that 13% of the posterior samples are stable for at least 10 Myr. The result from the stability analysis indicates that the two planets are trapped in a low-eccentricity 4:3 mean motion resonance. This is only the third discovered system to be inside a 4:3 resonance, making this discovery very valuable for planet formation and orbital evolution models.
Persistent Identifierhttp://hdl.handle.net/10722/286208
ISSN
2023 Impact Factor: 5.4
2023 SCImago Journal Rankings: 1.896
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorLuque, R-
dc.contributor.authorTrifonov, T-
dc.contributor.authorReffert, S-
dc.contributor.authorQuirrenbach, A-
dc.contributor.authorLee, MH-
dc.contributor.authorAlbrecht, S-
dc.contributor.authorFredslund Andersen, M-
dc.contributor.authorAntoci, V-
dc.contributor.authorGrundahl, F-
dc.contributor.authorSchwab, C-
dc.contributor.authorWolthoff, V-
dc.date.accessioned2020-08-31T07:00:40Z-
dc.date.available2020-08-31T07:00:40Z-
dc.date.issued2019-
dc.identifier.citationAstronomy & Astrophysics, 2019, v. 631, p. A136:1-A136:8-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/286208-
dc.description.abstractWe report the discovery of a second planet orbiting the K giant star 7 CMa based on 166 high-precision radial velocities obtained with Lick, HARPS, UCLES, and SONG. The periodogram analysis reveals two periodic signals of approximately 745 and 980 d, associated with planetary companions. A double-Keplerian orbital fit of the data reveals two Jupiter-like planets with minimum masses mb sini ~ 1.9 MJ and mc sini ~ 0.9 MJ, orbiting at semimajor axes of ab ~ 1.75 au and ac ~ 2.15 au, respectively. Given the small orbital separation and the large minimum masses of the planets, close encounters may occur within the time baseline of the observations; thus, a more accurate N-body dynamical modeling of the available data is performed. The dynamical best-fit solution leads to collision of the planets and we explore the long-term stable configuration of the system in a Bayesian framework, confirming that 13% of the posterior samples are stable for at least 10 Myr. The result from the stability analysis indicates that the two planets are trapped in a low-eccentricity 4:3 mean motion resonance. This is only the third discovered system to be inside a 4:3 resonance, making this discovery very valuable for planet formation and orbital evolution models.-
dc.languageeng-
dc.publisherEDP Sciences. The Journal's web site is located at http://www.aanda.org-
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsReproduced with permission from [Astronomy & Astrophysics], © [copyright holder] [2019]. The original publication is available at https://doi.org/10.1051/0004-6361/201936464-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.subjecttechniques: radial velocities-
dc.subjectplanetary systems-
dc.subjectplanets and satellites: dynamical evolution and stability-
dc.subjectplanets and satellites: detection-
dc.titlePrecise radial velocities of giant stars: XIII. A second Jupiter orbiting in 4:3 resonance in the 7 CMa system-
dc.typeArticle-
dc.identifier.emailLee, MH: mhlee@hku.hk-
dc.identifier.authorityLee, MH=rp00724-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1051/0004-6361/201936464-
dc.identifier.scopuseid_2-s2.0-85103739137-
dc.identifier.hkuros313330-
dc.identifier.volume631-
dc.identifier.spageA136:1-
dc.identifier.epageA136:8-
dc.identifier.isiWOS:000515099300005-
dc.publisher.placeFrance-
dc.identifier.issnl0004-6361-

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