Volume 522, November 2010
|Number of page(s)||10|
|Section||Planets and planetary systems|
|Published online||09 November 2010|
Transiting exoplanets from the CoRoT space mission⋆
XIII. CoRoT-13b: a dense hot Jupiter in transit around a star with solar metallicity and super-solar lithium content
Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2,
2 LUTH, Observatoire de Paris, UMR 8102 CNRS, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France
3 LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195 Meudon, France
4 Institut d’Astrophysique Spatiale, Université Paris XI, 91405 Orsay, France
5 Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France
6 Department of Physics, Denys Wilkinson Building Keble Road, Oxford, OX1 3RH, UK
7 Observatoire de l’Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
8 Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
9 Laboratoire d’Astrophysique de Marseille, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France
10 Observatoire de Haute Provence, 04670 Saint Michel l’Observatoire, France
11 Rheinisches Institut für Umweltforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Germany
12 Research and Scientific Support Department, ESTEC/ESA, PO Box 299, 2200 AG Noordwijk, The Netherlands
13 University of Vienna, Institute of Astronomy, Türkenschanzstr. 17, 1180 Vienna, Austria
14 IAG-Universidade de Sao Paulo, Brasil
15 Thüringer Landessternwarte, Sternwarte 5, Tautenburg 5, 07778 Tautenburg, Germany
16 Université de Nice-SophiaAntipolis, CNRS UMR 6202, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice Cedex 4, France
17 University of Liège, Allée du 6 août 17, Sart Tilman, Liège 1, Belgium
18 Space Research Institute, Austrian Academy of Science, Schmiedlstr. 6, 8042 Graz, Austria
19 School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv, Israel
20 Center for Astronomy and Astrophysics, TU Berlin, Hardenbergstr. 36, 10623 Berlin, Germany
Received: 4 June 2010
Accepted: 28 July 2010
We announce the discovery of the transiting planet CoRoT-13b. Ground-based follow-up in CFHT and IAC80 confirmed CoRoT’s observations. The mass of the planet was measured with the HARPS spectrograph and the properties of the host star were obtained analyzing HIRES spectra from the Keck telescope. It is a hot Jupiter-like planet with an orbital period of 4.04 days, 1.3 Jupiter masses, 0.9 Jupiter radii, and a density of 2.34 g cm-3. It orbits a G0V star with Teff = 5945 K, M∗ = 1.09 M⊙, R∗ = 1.01 R⊙, solar metallicity, a lithium content of + 1.45 dex, and an estimated age of between 0.12 and 3.15 Gyr. The lithium abundance of the star is consistent with its effective temperature, activity level, and age range derived from the stellar analysis. The density of the planet is extreme for its mass, implies that heavy elements are present with a mass of between about 140 and 300 M⊕.
Key words: planetary systems / techniques: photometric / techniques: radial velocities / techniques: spectroscopic
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. Part of the observations were obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Based on observations made with HARPS spectrograph on the 3.6-m European Organisation for Astronomical Research in the Southern Hemisphere telescope at La Silla Observatory, Chile (ESO program 184.C-0639). Based on observations made with the IAC80 telescope operated on the island of Tenerife by the Instituto de Astrofísica de Canarias in the Spanish Observatorio del Teide. Part of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
© ESO, 2010
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