Bibcode
Bouchy, F.; Deleuil, M.; Guillot, T.; Aigrain, S.; Carone, L.; Cochran, W. D.; Almenara, J. M.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.; Bonomo, A. S.; Bordé, P.; Csizmadia, Sz.; de Bondt, K.; Deeg, H. J.; Díaz, R. F.; Dvorak, R.; Endl, M.; Erikson, A.; Ferraz-Mello, S.; Fridlund, M.; Gandolfi, D.; Gazzano, J. C.; Gibson, N.; Gillon, M.; Guenther, E.; Hatzes, A.; Havel, M.; Hébrard, G.; Jorda, L.; Léger, A.; Lovis, C.; Llebaria, A.; Lammer, H.; MacQueen, P. J.; Mazeh, T.; Moutou, C.; Ofir, A.; Ollivier, M.; Parviainen, H.; Pätzold, M.; Queloz, D.; Rauer, H.; Rouan, D.; Santerne, A.; Schneider, J.; Tingley, B.; Wuchterl, G.
Bibliographical reference
Astronomy and Astrophysics, Volume 525, id.A68
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1
2011
Journal
Citations
96
Refereed citations
79
Description
We report the discovery by the CoRoT space mission of a transiting brown
dwarf orbiting a F7V star with an orbital period of 3.06 days. CoRoT-15b
has a radius of 1.12+0.30-0.15 {R}_Jup and a mass
of 63.3 ± 4.1 {M}_Jup, and is thus the second transiting
companion lying in the theoretical mass domain of brown dwarfs.
CoRoT-15b is either very young or inflated compared to standard
evolution models, a situation similar to that of M-dwarf stars orbiting
close to solar-type stars. Spectroscopic constraints and an analysis of
the lightcurve imply a spin period in the range 2.9-3.1 days for the
central star, which is compatible with a double-synchronisation of the
system.
The CoRoT space mission, launched on December 27th 2006, has been
developed and is operated by CNES, with the contribution of Austria,
Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain.
Observations made with HARPS spectrograph at ESO La Silla Observatory
(184.C-0639).
Related projects
Helio and Astero-Seismology and Exoplanets Search
The principal objectives of this project are: 1) to study the structure and dynamics of the solar interior, 2) to extend this study to other stars, 3) to search for extrasolar planets using photometric methods (primarily by transits of their host stars) and their characterization (using radial velocity information) and 4) the study of the planetary
Savita
Mathur