KELT-7b: A HOT JUPITER TRANSITING A BRIGHT V = 8.54 RAPIDLY ROTATING F-STAR
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Bieryla-2015-KELT-7b_ A HOT JUPIT.pdf
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1.52 MB
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Author(s)
Winn, Joshua Nathan
Date Issued
June 2015
Journal
The Astronomical Journal
Publisher
IOP Publishing
Citation
Bieryla, Allyson, Karen Collins, Thomas G. Beatty, Jason Eastman, Robert J. Siverd, Joshua Pepper, B. Scott Gaudi, et al. “KELT-7b: A HOT JUPITER TRANSITING A BRIGHT V = 8.54 RAPIDLY ROTATING F-STAR.” The Astronomical Journal 150, no. 1 (June 18, 2015): 12. © 2015 The American Astronomical Society
Version
Final published version
Abstract
We report the discovery of KELT-7b, a transiting hot Jupiter with a mass of 1.28 ± 0.18 M[subscript J], radius of 1.533[+0.046 over -0.047] R[subscript J], and an orbital period of 2.7347749 ± 0.0000039 days. The bright host star (HD 33643; KELT-7) is an F-star with V = 8.54, T[subscript eff] = 6789[+50 over -49] K, [Fe/H] = 0.139[+0.075 over -0.081], and log g = 4.149 ± 0.019]. It has a mass of 1.535 [+0.066 over -0.054] M[subscript ⊙], a radius of 1.732[+0.043 over -0.045] R[subscript ⊙], and is the fifth most massive, fifth hottest, and the ninth brightest star known to host a transiting planet. It is also the brightest star around which Kilodegree Extremely Little Telescope (KELT) has discovered a transiting planet. Thus, KELT-7b is an ideal target for detailed characterization given its relatively low surface gravity, high equilibrium temperature, and bright host star. The rapid rotation of the star (73 ± 0.5 km s[superscript −1]) results in a Rossiter–McLaughlin effect with an unusually large amplitude of several hundred m s[superscript −1]. We find that the orbit normal of the planet is likely to be well-aligned with the stellar spin axis, with a projected spin–orbit alignment of λ = 9[° over .]7 ± 5[° over .]2. This is currently the second most rapidly rotating star to have a reflex signal (and thus mass determination) due to a planetary companion measured.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-6256/150/1/12
