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Measurement of the nodal precession of WASP-33 b via doppler tomography

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Cameron_2015_TAJT_Measurement.pdf (524.4Kb)
Date
03/09/2015
Author
Johnson, Marshall C.
Cochran, William D.
Cameron, Andrew Collier
Bayliss, Daniel
Keywords
Line: profiles
Planet–star interactions
Planetary systems
Planets and satellites: individual (WASP-33 b)
Techniques: spectroscopic
QB Astronomy
QC Physics
DAS
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Abstract
We 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.
Citation
Johnson , 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/L23
Publication
Astrophysical Journal Letters
Status
Peer reviewed
DOI
https://doi.org/10.1088/2041-8205/810/2/L23
ISSN
2041-8205
Type
Journal article
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/L23
Description
M.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.
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  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2015arXiv150802398J
URI
http://hdl.handle.net/10023/7459

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