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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, S; West, R. G; Zhou, G
Monthly notices of the Royal Astronomical Society, 11/2017, Letnik: 471, Številka: 3Journal Article, Web Resource
Abstract 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 R Jup planet was confirmed by Doppler tomography of the stellar line profiles during transit. We place a limit of <8 M Jup 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.
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