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dc.contributor.authorJohnson, Marshall C.
dc.contributor.authorCochran, William D.
dc.contributor.authorCameron, Andrew Collier
dc.contributor.authorBayliss, Daniel
dc.date.accessioned2015-09-14T16:10:01Z
dc.date.available2015-09-14T16:10:01Z
dc.date.issued2015-09-03
dc.identifier.citationJohnson , M C , Cochran , W D , Cameron , A C & Bayliss , D 2015 , ' Measurement of the nodal precession of WASP-33 b via doppler tomography ' , Astrophysical Journal Letters , vol. 810 , no. 2 . https://doi.org/10.1088/2041-8205/810/2/L23en
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 209407259
dc.identifier.otherPURE UUID: 8801be4c-0366-46b5-9fd5-617e393cca8f
dc.identifier.otherBibCode: 2015arXiv150802398J
dc.identifier.otherScopus: 84941058980
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531438
dc.identifier.otherWOS: 000364340000010
dc.identifier.urihttp://hdl.handle.net/10023/7459
dc.descriptionM.C.J. is supported by a NASA Earth and Space Science Fellowship under Grant NNX12AL59H. This work was also supported by NASA Origins of Solar Systems Program grant NNX11AC34G to W.D.C.en
dc.description.abstractWe have analyzed new and archival time series spectra taken six years apart during transits of the hot Jupiter WASP-33 b, and spectroscopically resolved the line profile perturbation caused by the Rossiter–McLaughlin effect. The motion of this line profile perturbation is determined by the path of the planet across the stellar disk, which we show to have changed between the two epochs due to nodal precession of the planetary orbit. We measured rates of change of the impact parameter and the sky-projected spin–orbit misalignment of db/dt = -0.0228+0.0050-0.0018 yr-1 and dλ/dt = -0º.373+0.089-0.076 yr-1, respectively, corresponding to a rate of nodal precession of dΩ/dt =-0º.373+0.031-0.083 yr-1. This is only the second measurement of nodal precession for a confirmed exoplanet transiting a single star. Finally, we used the rate of precession to set limits on the stellar gravitational quadrupole moment of 0.0054≤ J2 ≤ 0.035.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rights© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/2041-8205/810/2/L23en
dc.subjectLine: profilesen
dc.subjectPlanet–star interactionsen
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: individual (WASP-33 b)en
dc.subjectTechniques: spectroscopicen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleMeasurement of the nodal precession of WASP-33 b via doppler tomographyen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/2041-8205/810/2/L23
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015arXiv150802398Jen


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