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Article: Precise radial velocities of giant stars XI: Two brown dwarfs in 6:1 mean motion resonance around the K giant star ν Ophiuch

TitlePrecise radial velocities of giant stars XI: Two brown dwarfs in 6:1 mean motion resonance around the K giant star ν Ophiuch
Authors
KeywordsTechniques: radial velocities
Planets and satellites: detection
Planets and satellites: dynamical evolution and stability
Brown dwarfs
Planetary systems
Issue Date2019
PublisherEDP Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy & Astrophysics, 2019, v. 624, article no. A18, p. 1-17 How to Cite?
AbstractWe present radial-velocity (RV) measurements for the K giant ν Oph (= HIP 88048, HD 163917, HR 6698), which reveal two brown dwarf companions with a period ratio close to 6:1. For our orbital analysis we use 150 precise RV measurements taken at the Lick Observatory between 2000 and 2011, and we combine them with RV data for this star available in the literature. Using a stellar mass of M = 2.7M⊙ for ν Oph and applying a self-consistent N-body model we estimate the minimum dynamical companion masses to be m1 sin i ≈ 22.2 MJup and m2 sin i ≈ 24.7 MJup, with orbital periods P1 ≈ 530 d and P2 ≈ 3185 d. We study a large set of potential orbital configurations for this system, employing a bootstrap analysis and a systematic χν2 grid-search coupled with our dynamical fitting model, and we examine their long-term stability. We find that the system is indeed locked in a 6:1 mean motion resonance (MMR), with Δω and all six resonance angles θ1–θ6 librating around 0°. We also test a large set of coplanar inclined configurations, and we find that the system will remain in a stable resonance for most of these configurations. The ν Oph system is important for probing planetary formation and evolution scenarios. It seems very likely that the two brown dwarf companions of ν Oph formed like planets in a circumstellar disk around the star and have been trapped in an MMR by smooth migration capture.
Persistent Identifierhttp://hdl.handle.net/10722/269342
ISSN
2023 Impact Factor: 5.4
2023 SCImago Journal Rankings: 1.896
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorQuirrenbach, A-
dc.contributor.authorTrifonov, TH-
dc.contributor.authorLee, MH-
dc.contributor.authorReffert, S-
dc.date.accessioned2019-04-24T08:05:43Z-
dc.date.available2019-04-24T08:05:43Z-
dc.date.issued2019-
dc.identifier.citationAstronomy & Astrophysics, 2019, v. 624, article no. A18, p. 1-17-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/269342-
dc.description.abstractWe present radial-velocity (RV) measurements for the K giant ν Oph (= HIP 88048, HD 163917, HR 6698), which reveal two brown dwarf companions with a period ratio close to 6:1. For our orbital analysis we use 150 precise RV measurements taken at the Lick Observatory between 2000 and 2011, and we combine them with RV data for this star available in the literature. Using a stellar mass of M = 2.7M⊙ for ν Oph and applying a self-consistent N-body model we estimate the minimum dynamical companion masses to be m1 sin i ≈ 22.2 MJup and m2 sin i ≈ 24.7 MJup, with orbital periods P1 ≈ 530 d and P2 ≈ 3185 d. We study a large set of potential orbital configurations for this system, employing a bootstrap analysis and a systematic χν2 grid-search coupled with our dynamical fitting model, and we examine their long-term stability. We find that the system is indeed locked in a 6:1 mean motion resonance (MMR), with Δω and all six resonance angles θ1–θ6 librating around 0°. We also test a large set of coplanar inclined configurations, and we find that the system will remain in a stable resonance for most of these configurations. The ν Oph system is important for probing planetary formation and evolution scenarios. It seems very likely that the two brown dwarf companions of ν Oph formed like planets in a circumstellar disk around the star and have been trapped in an MMR by smooth migration capture.-
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, © ESO 2019. The original publication is available at https://doi.org/10.1051/0004-6361/201834423-
dc.subjectTechniques: radial velocities-
dc.subjectPlanets and satellites: detection-
dc.subjectPlanets and satellites: dynamical evolution and stability-
dc.subjectBrown dwarfs-
dc.subjectPlanetary systems-
dc.titlePrecise radial velocities of giant stars XI: Two brown dwarfs in 6:1 mean motion resonance around the K giant star ν Ophiuch-
dc.typeArticle-
dc.identifier.emailLee, MH: mhlee@hku.hk-
dc.identifier.authorityLee, MH=rp00724-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1051/0004-6361/201834423-
dc.identifier.scopuseid_2-s2.0-85063863163-
dc.identifier.hkuros297618-
dc.identifier.volume624-
dc.identifier.spagearticle no. A18, p. 1-
dc.identifier.epagearticle no. A18, p. 17-
dc.identifier.isiWOS:000462979700001-
dc.publisher.placeFrance-
dc.identifier.issnl0004-6361-

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