WASP-167b/KELT-13b : joint discovery of a hot Jupiter transiting a rapidly rotating F1V star
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We report the joint WASP/KELT discovery of WASP-167b/KELT-13b, a transiting hot Jupiter with a 2.02-d orbit around a V = 10.5, F1V star with [Fe/H] = 0.1 ± 0.1. The 1.5 RJup planet was confirmed by Doppler tomography of the stellar line profiles during transit. We place a limit of <8 MJup on its mass. The planet is in a retrograde orbit with a sky-projected spin–orbit angle of λ = −165° ± 5°. This is in agreement with the known tendency for orbits around hotter stars to be more likely to be misaligned. WASP-167/KELT-13 is one of the few systems where the stellar rotation period is less than the planetary orbital period. We find evidence of non-radial stellar pulsations in the host star, making it a δ-Scuti or γ-Dor variable. The similarity to WASP-33, a previously known hot-Jupiter host with pulsations, adds to the suggestion that close-in planets might be able to excite stellar pulsations.
Temple , L Y , Hellier , C , Albrow , M D , Anderson , D R , Bayliss , D , Beatty , T G , Bieryla , A , Brown , D J A , Cargile , P A , Collier Cameron , A , Collins , K A , Colón , K D , Curtis , I A , D'Ago , G , Delrez , L , Eastman , J , Gaudi , B S , Gillon , M , Gregorio , J , James , D , Jehin , E , Joner , M D , Kielkopf , J F , Kuhn , R B , Labadie-Bartz , J , Latham , D W , Lendl , M , Lund , M B , Malpas , A L , Maxted , P F L , Myers , G , Oberst , T E , Pepe , F , Pepper , J , Pollacco , D , Queloz , D , Rodriguez , J E , Ségransan , D , Siverd , R J , Smalley , B , Stassun , K G , Stevens , D J , Stockdale , C , Tan , T G , Triaud , A H M J , Udry , S , Villanueva, Jr. , S , West , R G & Zhou , G 2017 , ' WASP-167b/KELT-13b : joint discovery of a hot Jupiter transiting a rapidly rotating F1V star ' Monthly Notices of the Royal Astronomical Society , vol 471 , no. 3 , pp. 2743-2752 . DOI: 10.1093/mnras/stx1729
Monthly Notices of the Royal Astronomical Society
© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. 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: https://doi.org/10.1093/mnras/stx1729
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