Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47
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We report the discovery of two additional planetary companions to WASP-41 and WASP-47. WASP-41 c is a planet of minimum mass 3.18 ± 0.20 MJup and eccentricity 0.29 ± 0.02, and it orbits in 421 ± 2 days. WASP-47 c is a planet of minimum mass 1.24 ± 0.22 MJup and eccentricity 0.13 ± 0.10, and it orbits in 572 ± 7 days. Unlike most of the planetary systems that include a hot Jupiter, these two systems with a hot Jupiter have a long-period planet located at only ~1 au from their host star. WASP-41 is a rather young star known to be chromospherically active. To differentiate its magnetic cycle from the radial velocity effect induced by the second planet, we used the emission in the Hα line and find this indicator well suited to detecting the stellar activity pattern and the magnetic cycle. The analysis of the Rossiter-McLaughlin effect induced by WASP-41 b suggests that the planet could be misaligned, though an aligned orbit cannot be excluded. WASP-47 has recently been found to host two additional transiting super Earths. With such an unprecedented architecture, the WASP-47 system will be very important for understanding planetary migration.
Neveu-VanMalle , M , Queloz , D , Anderson , D R , Brown , D J A , Cameron , A C , Delrez , L , Díaz , R F , Gillon , M , Hellier , C , Jehin , E , Lister , T A , Pepe , F , Rojo , P , Ségransan , D , Triaud , A H M J , Turner , O D & Udry , S 2016 , ' Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47 ' Astronomy & Astrophysics , vol. 586 , A93 . DOI: 10.1051/0004-6361/201526965
Astronomy & Astrophysics
© ESO, 2016. 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/10.1051/0004-6361/201526965. Reproduced with permission from Astronomy & Astrophysics, © ESO.
DescriptionTRAPPIST is a project funded by the Belgian Fund for Scientic Research (Fonds National de la Recherche Scientique, F.R.S.-FNRS) under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF). L. Delrez acknowledges support of the F.R.I.A. fund of the FNRS. M. Gillon and E. Jehin are FNRS Research Associates. A.C.C. and C.H. acknowledge support from STFC grants ST/M001296/1 and ST/J001384/1 respectively.
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