Volume 502, Number 1, July IV 2009
|Page(s)||391 - 394|
|Section||Planets and planetary systems|
|Published online||19 May 2009|
The 0.5MJ transiting exoplanet WASP-13b*
Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700 Santa Cruz de la Palma, Tenerife, Spain e-mail: email@example.com
2 Astrophysics Research Centre, School of Mathematics & Physics, Queen's University, University Road, Belfast, BT7 1NN, UK
3 School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK
4 Institut d'Astrophysique de Paris, CNRS (UMR 7095) – Université Pierre & Marie Curie, 98 bvd. Arago, 75014 Paris, France
5 Observatoire de Haute-Provence, 04870 St Michel l'Observatoire, France
6 Department of Physics and Astronomy, California State University, 18111 Nordhoff Street, Northridge, CA, USA
7 Laboratoire d'Astrophysique de Marseille, BP 8, 13376 Marseille Cedex 12, France
8 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK
9 Las Cumbres Observatory, 6740 Cortona Dr. Suite 102, Santa Barbara, CA 93117, USA
10 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
11 Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK
12 Department of Physics and Astronomy, The Open University, Milton Keynes, MK7 6AA, UK
13 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
14 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
15 Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent, CT2 7NH, UK
Accepted: 12 May 2009
We report the discovery of WASP-13b, a low-mass transiting exoplanet with an orbital period of 4.35298 ± 0.00004 days. The transit has a depth of 9 mmag, and although our follow-up photometry does not allow us to constrain the impact parameter well (0 < b < 0.46), with radius in the range Rp ~ 1.06-1.21 RJ the location of WASP-13b in the mass-radius plane is nevertheless consistent with H/He-dominated, irradiated, low core mass and core-free theoretical models. The G1V host star is similar to the Sun in mass and metallicity ([M/H] = 0.0±0.2), but is possibly older ( Gyr).
Key words: binaries: eclipsing / planetary systems / techniques: photometric / techniques: radial velocities / techniques: spectroscopic / stars: individual: WASP-13b
© ESO, 2009
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