Transiting exoplanets from the CoRoT space mission : XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets

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作者
Almenara, J.M. [1 ]
Bouchy, F. [1 ,2 ]
Gaulme, P. [3 ]
Deleuil, M. [1 ]
Havel, M. [4 ]
Gandolfi, D. [5 ]
Deeg, H.J. [6 ,7 ]
Wuchterl, G. [8 ]
Guillot, T. [9 ]
Gardes, B. [1 ]
Pasternacki, T. [10 ]
Aigrain, S. [11 ]
Alonso, R. [6 ,7 ,12 ]
Auvergne, M. [13 ]
Baglin, A. [13 ]
Bonomo, A.S. [1 ,14 ]
Bordé, P. [15 ]
Cabrera, J. [10 ]
Carpano, S. [5 ]
Cochran, W.D. [16 ]
Csizmadia, Sz. [10 ]
Damiani, C. [1 ]
Diaz, R.F. [1 ]
Dvorak, R. [17 ]
Endl, M. [16 ]
Erikson, A. [10 ]
Ferraz-Mello, S. [18 ]
Fridlund, M. [5 ]
Hébrard, G. [2 ,19 ]
Gillon, M. [20 ]
Guenther, E. [8 ]
Hatzes, A. [8 ]
Léger, A. [15 ]
Lammer, H. [21 ]
MacQueen, P.J. [16 ]
Mazeh, T. [22 ]
Moutou, C. [1 ]
Ollivier, M. [15 ]
Ofir, A. [23 ]
Pätzold, M. [24 ]
Parviainen, H. [6 ,7 ]
Queloz, D. [12 ]
Rauer, H. [10 ,25 ]
Rouan, D. [13 ]
Santerne, A. [1 ]
Samuel, B. [13 ]
Schneider, J. [26 ]
Tal-Or, L. [22 ]
Tingley, B. [6 ,7 ,27 ]
Weingrill, J. [21 ]
机构
[1] Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326
[2] Institut d'Astrophysique de Paris, 75014 Paris
[3] Department of Astronomy, New Mexico State University, Las Cruces, NM 88003-8001
[4] NASA Postdoctoral Program Fellow, Ames Research Center, Moffett Field, CA 94035
[5] Research and Scientific Support Department, ESTEC/ESA, 2200 AG Noordwijk
[6] Instituto de Astrofisica de Canarias, 38205 La Laguna, Tenerife
[7] Universidad de la Laguna, Dept. de Astrofísica, 38200 La Laguna, Tenerife
[8] Thüringer Landessternwarte, Tautenburg 5, 07778 Tautenburg
[9] Observatoire de la Côte d'Azur, Laboratoire Cassiopée, 06304 Nice Cedex 4
[10] Institute of Planetary Research, German Aerospace Center, 12489 Berlin
[11] Department of Physics, Denys Wilkinson Building, Oxford, OX1 3RH, Keble Road
[12] Observatoire de l'Université de Genève, 1290 Sauverny
[13] LESIA, Obs de Paris, 92195 Meudon cedex, Place J. Janssen
[14] INAF-Osservatorio Astronomico di Torino, 10025 Pino Torinese
[15] Institut d'Astrophysique Spatiale, Université Paris-Sud 11 and CNRS, UMR 8617, 91405 Orsay
[16] McDonald Observatory, University of Texas at Austin, Austin
[17] University of Vienna, Institute of Astronomy, 1180 Vienna
[18] IAG, Universidade de Sao Paulo
[19] Observatoire de Haute Provence
[20] University of Liège, Sart Tilman, Liège 1
[21] Space Research Institute, Austrian Academy of Science, 8042 Graz
[22] Wise Observatory, Tel Aviv University
[23] Institut für Astrophysik, Georg-August-Universität, 37077 Göttingen
[24] Rheinisches Institut für Umweltforschung An der Universität zu Köln, 50931 Köln
[25] Center for Astronomy and Astrophysics, TU Berlin, 10623 Berlin
[26] LUTH, CNRS, Université Paris Diderot, 92195 Meudon
[27] Department of Physics and Astronomy, Aarhus University
基金
英国科学技术设施理事会; 美国国家航空航天局;
关键词
Planetary systems; Techniques: photometric; Techniques: radial velocities; Techniques: spectroscopic;
D O I
10.1051/0004-6361/201321462
中图分类号
学科分类号
摘要
We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 MJup, a radius of 1.08 -0.10+0.3 RJup and hence a mean density of 0.15-0.06+0.15 g cm-3. The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0+1.8-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 MJup, a radius of 1.26-0.07+0.13 RJup, and a mean density of 0.28-0.07+0.09 g cm-3, it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 -0.15+0.08 and 0.26-0.08+0.05, respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size. © 2013 ESO.
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