File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: On the 2:1 Orbital resonance in the HD 82943 planetary system

TitleOn the 2:1 Orbital resonance in the HD 82943 planetary system
Authors
KeywordsCelestial Mechanics
Planetary Systems
Stars: Individual (Hd 82943)
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 641 n. 2 I, p. 1178-1187 How to Cite?
AbstractWe present an analysis of the HD 82943 planetary system based on a radial velocity data set that combines new measurements obtained with the Keck telescope and the CORALIE measurements published in graphical form. We examine simultaneously the goodness of fit and the dynamical properties of the best-fit double-Keplerian model as a function of the poorly constrained eccentricity and argument of periapse of the outer planet's orbit. The fit with the minimum χ v 2 is dynamically unstable if the orbits are assumed to be coplanar. However, the minimum is relatively shallow, and there is a wide range of fits outside the minimum with reasonable χ v 2, For an assumed coplanar inclination i = 30° (sin i = 0.5), only good fits with both of the lowest order, eccentricity-type mean-motion resonance variables at the 2:1 commensurability, θ 1 and θ 2, librating about 0° are stable. For sin i = 1, there are also some good fits with only θ 1 (involving the inner planet's periapse longitude) librating that are stable for at least 10 8 yr. The libration semiamplitudes are about 6° for θ 1 and 10° for θ 2 for the stable good fit with the smallest libration amplitudes of both θ 1 and θ 2. We do not find any good fits that are nonresonant and stable. Thus, the two planets in the HD 82943 system are almost certainly in 2:1 mean-motion resonance, with at least θ 1 librating, and the observations may even be consistent with small-amplitude librations of both θ 1 and θ 2. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/151189
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLee, MHen_US
dc.contributor.authorPaul Butler, Ren_US
dc.contributor.authorFischer, DAen_US
dc.contributor.authorMarcy, GWen_US
dc.contributor.authorVogt, SSen_US
dc.date.accessioned2012-06-26T06:18:27Z-
dc.date.available2012-06-26T06:18:27Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 641 n. 2 I, p. 1178-1187en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/151189-
dc.description.abstractWe present an analysis of the HD 82943 planetary system based on a radial velocity data set that combines new measurements obtained with the Keck telescope and the CORALIE measurements published in graphical form. We examine simultaneously the goodness of fit and the dynamical properties of the best-fit double-Keplerian model as a function of the poorly constrained eccentricity and argument of periapse of the outer planet's orbit. The fit with the minimum χ v 2 is dynamically unstable if the orbits are assumed to be coplanar. However, the minimum is relatively shallow, and there is a wide range of fits outside the minimum with reasonable χ v 2, For an assumed coplanar inclination i = 30° (sin i = 0.5), only good fits with both of the lowest order, eccentricity-type mean-motion resonance variables at the 2:1 commensurability, θ 1 and θ 2, librating about 0° are stable. For sin i = 1, there are also some good fits with only θ 1 (involving the inner planet's periapse longitude) librating that are stable for at least 10 8 yr. The libration semiamplitudes are about 6° for θ 1 and 10° for θ 2 for the stable good fit with the smallest libration amplitudes of both θ 1 and θ 2. We do not find any good fits that are nonresonant and stable. Thus, the two planets in the HD 82943 system are almost certainly in 2:1 mean-motion resonance, with at least θ 1 librating, and the observations may even be consistent with small-amplitude librations of both θ 1 and θ 2. © 2006. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectCelestial Mechanicsen_US
dc.subjectPlanetary Systemsen_US
dc.subjectStars: Individual (Hd 82943)en_US
dc.titleOn the 2:1 Orbital resonance in the HD 82943 planetary systemen_US
dc.typeArticleen_US
dc.identifier.emailLee, MH:mhlee@hku.hken_US
dc.identifier.authorityLee, MH=rp00724en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/500566en_US
dc.identifier.scopuseid_2-s2.0-33745324516en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33745324516&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume641en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage1178en_US
dc.identifier.epage1187en_US
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000236819400048-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLee, MH=7409119699en_US
dc.identifier.scopusauthoridPaul Butler, R=7401524951en_US
dc.identifier.scopusauthoridFischer, DA=7402948435en_US
dc.identifier.scopusauthoridMarcy, GW=7005624592en_US
dc.identifier.scopusauthoridVogt, SS=7101896528en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats