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dc.creatorRobertson, Paulen_US
dc.creatorHorner, Jonathanen_US
dc.creatorWittenmyer, Robert A.en_US
dc.creatorEndl, Michaelen_US
dc.creatorCochran, William D.en_US
dc.creatorMacQueen, Phillip J.en_US
dc.creatorBrugamyer, Erik J.en_US
dc.creatorSimon, Attila E.en_US
dc.creatorBarnes, Stuart I.en_US
dc.creatorCaldwell, Carolineen_US
dc.date.accessioned2016-04-28T19:32:19Z
dc.date.available2016-04-28T19:32:19Z
dc.date.issued2012-07en
dc.identifierdoi:10.15781/T2K803
dc.identifier.citationRobertson, Paul, J. Horner, Robert A. Wittenmyer, Michael Endl, William D. Cochran, Phillip J. MacQueen, Erik J. Brugamyer, Attila E. Simon, Stuart I. Barnes, and Caroline Caldwell. "A second giant planet in 3: 2 mean-motion resonance in the HD 204313 system." The Astrophysical Journal, Vol. 754, No. 1 (Jul., 2012): 50.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34675
dc.description.abstractWe present eight years of high-precision radial velocity (RV) data for HD 204313 from the 2.7 m Harlan J. Smith Telescope at McDonald Observatory. The star is known to have a giant planet (M sin i = 3.5 M-J) on a similar to 1900 day orbit, and a Neptune-mass planet at 0.2 AU. Using our own data in combination with the published CORALIE RVs of Segransan et al., we discover an outer Jovian (M sin i = 1.6 M-J) planet with P similar to 2800 days. Our orbital fit suggests that the planets are in a 3: 2 mean motion resonance, which would potentially affect their stability. We perform a detailed stability analysis and verify that the planets must be in resonance.en_US
dc.description.sponsorshipAustralian government through ARC DP0774000en_US
dc.description.sponsorshipUNSWen_US
dc.description.sponsorshipNational Aeronautics and Space Administration NNX07AL70G, NNX09AB30Gen_US
dc.description.sponsorshipHungarian OTKA K76816, K83790, MB08C 81013en_US
dc.description.sponsorshipHungarian Academy of Scienceen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectplanetary systemsen_US
dc.subjectplanets and satellites: dynamical evolution anden_US
dc.subjectstabilityen_US
dc.subjectstars: individual (hd 204313)en_US
dc.subjecttechniques: radial velocitiesen_US
dc.subjectsolar-systemen_US
dc.subjecttiming variationsen_US
dc.subjecttrojan asteroidsen_US
dc.subjectsearch programen_US
dc.subjectlong-perioden_US
dc.subjectlow-massen_US
dc.subjectstarsen_US
dc.subjectjupitersen_US
dc.subjectspectrometeren_US
dc.subjectstabilityen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleA Second Giant Planet In 3:2 Mean-Motion Resonance In The HD 204313 Systemen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2012_07_secondgiant.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/754/1/50en_US
dc.contributor.utaustinauthorRobertson, Paulen_US
dc.contributor.utaustinauthorEndl, Michaelen_US
dc.contributor.utaustinauthorCochran, William D.en_US
dc.contributor.utaustinauthorMacQueen, Phillip J.en_US
dc.contributor.utaustinauthorBrugamyer, Erik J.en_US
dc.contributor.utaustinauthorBarnes, Stuart I.en_US
dc.contributor.utaustinauthorCaldwell, Carolineen_US
dc.relation.ispartofserialAstrophysical Journalen_US


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