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Title:
Transiting exoplanets from the CoRoT space mission. II. CoRoT-Exo-2b: a transiting planet around an active G star
Authors:
Alonso, R.; Auvergne, M.; Baglin, A.; Ollivier, M.; Moutou, C.; Rouan, D.; Deeg, H. J.; Aigrain, S.; Almenara, J. M.; Barbieri, M.; Barge, P.; Benz, W.; Bordé, P.; Bouchy, F.; de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gillon, M.; Gondoin, P.; Guillot, T.; Hatzes, A.; Hébrard, G.; Kabath, P.; Jorda, L.; Lammer, H.; Léger, A.; Llebaria, A.; Loeillet, B.; Magain, P.; Mayor, M.; Mazeh, T.; Pätzold, M.; Pepe, F.; Pont, F.; Queloz, D.; Rauer, H.; Shporer, A.; Schneider, J.; Stecklum, B.; Udry, S.; Wuchterl, G.
Affiliation:
AA(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France ), AB(LESIA, CNRS UMR 8109, Observatoire de Paris, 5 place J. Janssen, 92195 Meudon, France), AC(LESIA, CNRS UMR 8109, Observatoire de Paris, 5 place J. Janssen, 92195 Meudon, France), AD(IAS, Université Paris XI, 91405 Orsay, France), AE(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), AF(LESIA, CNRS UMR 8109, Observatoire de Paris, 5 place J. Janssen, 92195 Meudon, France), AG(Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain), AH(School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK), AI(Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain), AJ(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), AK(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), AL(Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland), AM(IAS, Université Paris XI, 91405 Orsay, France), AN(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France), AO(Observatório Nacional, Rio de Janeiro, RJ, Brazil), AP(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), AQ(Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria), AR(Institute of Planetary Research, DLR, Rutherfordstr. 2, 12489 Berlin, Germany), AS(Research and Scientific Support Department, European Space Agency, ESTEC, 2200 Noordwijk, The Netherlands), AT(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), AU(Research and Scientific Support Department, European Space Agency, ESTEC, 2200 Noordwijk, The Netherlands), AV(Observatoire de la Côte d'Azur, Laboratoire Cassiopée, CNRS UMR 6202, BP 4229, 06304 Nice Cedex 4, France), AW(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany), AX(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France), AY(Institute of Planetary Research, DLR, Rutherfordstr. 2, 12489 Berlin, Germany), AZ(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), BA(Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria), BB(IAS, Université Paris XI, 91405 Orsay, France), BC(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), BD(Laboratoire d'Astrophysique de Marseille, UMR 6110, CNRS/Université de Provence, Traverse du Siphon, 13376 Marseille, France), BE(Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 août 17, Sart Tilman, Liège 1, Belgium), BF(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), BG(School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel), BH(Rheinisches Institut für Umweltforschung, Universität zu Köln, Abt. Planetenforschung, Aachener Str. 209, 50931 Köln, Germany), BI(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), BJ(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), BK(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), BL(Institute of Planetary Research, DLR, Rutherfordstr. 2, 12489 Berlin, Germany; Center for Astronomy and Astrophysics, TU Berlin, Hardenbergstr. 36, 10623 Berlin, Germany), BM(School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel), BN(LUTH, Observatoire de Paris-Meudon, 5 place J. Janssen, 92195 Meudon, France), BO(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany), BP(Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland), BQ(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany)
Publication:
Astronomy and Astrophysics, Volume 482, Issue 3, 2008, pp.L21-L24 (A&A Homepage)
Publication Date:
05/2008
Origin:
EDP Sciences
Astronomy Keywords:
stars: planetary systems, techniques: photometric, techniques: radial velocity
DOI:
10.1051/0004-6361:200809431
Bibliographic Code:
2008A&A...482L..21A

Abstract

Context: The CoRoT mission, a pioneer in exoplanet searches from space, has completed its first 150 days of continuous observations of ~12 000 stars in the galactic plane. An analysis of the raw data identifies the most promising candidates and triggers the ground-based follow-up.
Aims: We report on the discovery of the transiting planet CoRoT-Exo-2b, with a period of 1.743 days, and characterize its main parameters.
Methods: We filter the CoRoT raw light curve of cosmic impacts, orbital residuals, and low frequency signals from the star. The folded light curve of 78 transits is fitted to a model to obtain the main parameters. Radial velocity data obtained with the SOPHIE, CORALIE and HARPS spectrographs are combined to characterize the system. The 2.5 min binned phase-folded light curve is affected by the effect of sucessive occultations of stellar active regions by the planet, and the dispersion in the out of transit part reaches a level of 1.09×10-4 in flux units.
Results: We derive a radius for the planet of 1.465 ± 0.029 R_Jup and a mass of 3.31 ± 0.16 M_Jup, corresponding to a density of 1.31 ± 0.04 g/cm^3. The large radius of CoRoT-Exo-2b cannot be explained by current models of evolution of irradiated planets.

Based on observations obtained with CoRoT, a space project operated by the French Space Agency, CNES, with participation of the Science Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany and Spain; and on observations made with SOPHIE spectrograph at Observatoire de Haute Provence, France (PNP.07 A.MOUT), CORALIE, and HARPS spectrograph at ESO La Silla Observatroy (079.C-0127/F)).

Table 2 is only available in electronic form at http://www.aanda.org


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