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dc.contributor.authorAlbrecht, Simon H.
dc.contributor.authorMarcy, Geoffrey W.
dc.contributor.authorHoward, Andrew W.
dc.contributor.authorIsaacson, Howard
dc.contributor.authorJohnson, John Asher
dc.contributor.authorWinn, Joshua Nathan
dc.date.accessioned2014-09-09T14:59:18Z
dc.date.available2014-09-09T14:59:18Z
dc.date.issued2013-06
dc.date.submitted2013-02
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/89225
dc.description.abstractWe measure the sky-projected stellar obliquities (λ) in the multiple-transiting planetary systems KOI-94 and Kepler-25, using the Rossiter-McLaughlin effect. In both cases, the host stars are well aligned with the orbital planes of the planets. For KOI-94 we find λ = –11° ± 11°, confirming a recent result by Hirano and coworkers. Kepler-25 was a more challenging case, because the transit depth is unusually small (0.13%). To obtain the obliquity, it was necessary to use prior knowledge of the star's projected rotation rate and apply two different analysis methods to independent wavelength regions of the spectra. The two methods gave consistent results, λ = 7° ± 8° and –0[° over .]5 ± 5[° over .]7. There are now a total of five obliquity measurements for host stars of systems of multiple-transiting planets, all of which are consistent with spin-orbit alignment. This alignment is unlikely to be the result of tidal interactions because of the relatively large orbital distances and low planetary masses in the systems. In this respect, the multiplanet host stars differ from hot-Jupiter host stars, which commonly have large spin-orbit misalignments whenever tidal interactions are weak. In particular, the weak-tide subset of hot-Jupiter hosts has obliquities consistent with an isotropic distribution (p = 0.6), but the multiplanet hosts are incompatible with such a distribution (p ~ 10[superscript –6]). This suggests that high obliquities are confined to hot-Jupiter systems, and provides further evidence that hot-Jupiter formation involves processes that tilt the planetary orbit.en_US
dc.description.sponsorshipUnited States. National Aeronautics and Space Administration (Origins Award NNX09AB33G)en_US
dc.description.sponsorshipNational Science Foundation (U.S.) (Grant 1108595)en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637X/771/1/11en_US
dc.rightsCreative Commons Attribution-Noncommercial-Share Alikeen_US
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/4.0/en_US
dc.sourcearXiven_US
dc.titleLOW STELLAR OBLIQUITIES IN COMPACT MULTIPLANET SYSTEMSen_US
dc.typeArticleen_US
dc.identifier.citationAlbrecht, Simon, Joshua N. Winn, Geoffrey W. Marcy, Andrew W. Howard, Howard Isaacson, and John A. Johnson. “LOW STELLAR OBLIQUITIES IN COMPACT MULTIPLANET SYSTEMS.” The Astrophysical Journal 771, no. 1 (June 10, 2013): 11.en_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorAlbrecht, Simon H.en_US
dc.contributor.mitauthorWinn, Joshua Nathanen_US
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsAlbrecht, Simon; Winn, Joshua N.; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard; Johnson, John A.en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-4265-047X
dspace.mitauthor.errortrue
mit.licenseOPEN_ACCESS_POLICYen_US
mit.metadata.statusComplete


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