A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY
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Johnson-2014-A misaligned prograd.pdf
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Author(s)
Johnson, Marshall C.
Cochran, William D.
Albrecht, Simon H.
Dodson-Robinson, Sarah E.
Gullikson, Kevin
Winn, Joshua Nathan
Date Issued
June 2014
Journal
Astrophysical Journal
Publisher
IOP Publishing
Citation
Johnson, Marshall C., William D. Cochran, Simon Albrecht, Sarah E. Dodson-Robinson, Joshua N. Winn, and Kevin Gullikson. “A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY.” The Astrophysical Journal 790, no. 1 (June 30, 2014): 30. © 2014 The American Astronomical Society.
Version
Final published version
Abstract
Transiting planets around rapidly rotating stars are not amenable to precise radial velocity observations, such as are used for planet candidate validation, as they have wide, rotationally broadened stellar lines. Such planets can, however, be observed using Doppler tomography, wherein stellar absorption line profile distortions during transit are spectroscopically resolved. This allows the validation of transiting planet candidates and the measurement of the stellar spin-planetary orbit (mis)alignment, which is an important statistical probe of planetary migration processes. We present Doppler tomographic observations that provide direct confirmation of the hot Jupiter Kepler-13 Ab and also show that the planet has a prograde, misaligned orbit with λ = 58°.6 ± 2°.0. Our measured value of the spin–orbit misalignment is in significant disagreement with the value of λ = 23° ± 4° previously measured by Barnes et al. (2011) from the gravity-darkened Kepler light curve. We also place an upper limit of 0.75 M☉ (95% confidence) on the mass of Kepler-13 C, the spectroscopic companion to Kepler-13 B, which is the proper-motion companion of the planet host star Kepler-13 A.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
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DOI of Published Version
https://doi.org/10.1088/0004-637X/790/1/30
