Transiting exoplanets from the CoRoT space mission: XXIX. The hot Jupiters CoRoT-30 b and CoRoT-31 b

• Autores: Bordé, P.; Diaz, Rodrigo Fernando; Creevey, O.; Damiani, C.; Deeg, H.; Klagyivik, P.; Wuchterl, G.; Gandolfi, D.; Fridlund, M.; Bouchy, F.; Aigrain, S.; Alonso, R.; Almenara, J. M.; Baglin, A.; Barros, S.C.C.; Bonomo, A.S.; Cabrera, J.; Csizmadia, Sz.; Deleuil, M.; Erikson, A.; Ferraz Mello, S.; Guenther, E.W.; Guillot, T.; Grziwa, S.; Hatzes, A.; Hébrard, G.; Mazeh, T.; Ollivier, M.; Parviainen, H.; Pätzold, M.; Rauer, H.; Rouan, D.; Santerne, A.; Schneider, J.
• Año de publicación: 2020
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: PLANETARY SYSTEMS; STARS: FUNDAMENTAL PARAMETERS; STARS: INDIVIDUAL: COROT-30; STARS: INDIVIDUAL: COROT-31
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

Aims. We report the discovery as well as the orbital and physical characterizations of two new transiting giant exoplanets, CoRoT-30 b and CoRoT-31 b, with the CoRoT space telescope. Methods. We analyzed two complementary data sets: photometric transit light curves measured by CoRoT, and radial velocity curves measured by the HARPS spectrometer. To derive the absolute masses and radii of the planets, we modeled the stars from available magnitudes and spectra. Results. We find that CoRoT-30 b is a warm Jupiter on a close-to-circular 9.06-day orbit around a G3V star with a semi-major axis of about 0.08 AU. It has a radius of 1.01 ± 0.08 RJ, a mass of 2.90 ± 0.22 MJ, and therefore a mean density of 3.45 ± 0.65 g cm-3. The hot Jupiter CoRoT-31 b is on a close-to-circular 4.63-day orbit around a G2 IV star with a semi-major axis of about 0.05 AU. It has a radius of 1.46 ± 0.30 RJ, a mass of 0.84 ± 0.34 MJ, and therefore a mean density of 0.33 ± 0.18 g cm-3. Conclusions. Neither system seems to support the claim that stars hosting planets are more depleted in lithium. The radii of both planets are close to that of Jupiter, but they differ in mass; CoRoT-30 b is ten times denser than CoRoT-31 b. The core of CoRoT-30 b would weigh between 15 and 75 Earth masses, whereas relatively weak constraints favor no core for CoRoT-31 b. In terms of evolution, the characteristics of CoRoT-31 b appear to be compatible with the high-eccentricity migration scenario, which is not the case for CoRoT-30 b. The angular momentum of CoRoT-31 b is currently too low for the planet to evolve toward synchronization of its orbital revolution with stellar rotation, and the planet will slowly spiral-in while its host star becomes a red giant. CoRoT-30 b is not synchronized either: it looses angular momentum owing to stellar winds and is expected reach steady state in about 2 Gyr. CoRoT-30 and 31, as a pair, are a truly remarkable example of diversity in systems with hot Jupiters.
Fil: Bordé, P.. Universite de Bordeaux; Francia
Fil: Diaz, Rodrigo Fernando. Universidad de Ginebra; Suiza. Universidad de Buenos Aires; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Creevey, O.. Institut D'astrophysique Spatiale; Francia. Université Côte d’Azur; Francia
Fil: Damiani, C.. Institut D'astrophysique Spatiale; Francia. Max Planck Institute For Solar System Research; Alemania
Fil: Deeg, H.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Klagyivik, P.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Wuchterl, G.. Kuffner Observatory; Austria
Fil: Gandolfi, D.. Università di Torino; Italia. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Fridlund, M.. Max Planck Institute For Astronomy; Alemania. Chalmers University of Technology; Suecia. Leiden University; Países Bajos
Fil: Bouchy, F.. Aix Marseille Université; Francia. Universidad de Ginebra; Suiza
Fil: Aigrain, S.. University of Oxford; Reino Unido
Fil: Alonso, R.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Almenara, J. M.. Universidad de Ginebra; Suiza. Aix Marseille Université; Francia
Fil: Baglin, A.. Université Pierre et Marie Curie; Francia
Fil: Barros, S.C.C.. Aix Marseille Université; Francia. Universidad de Porto; Portugal
Fil: Bonomo, A.S.. Istituto Nazionale di Astrofisica; Italia
Fil: Cabrera, J.. German Aerospace Center; Alemania
Fil: Csizmadia, Sz.. German Aerospace Center; Alemania
Fil: Deleuil, M.. Aix Marseille Université; Francia
Fil: Erikson, A.. German Aerospace Center; Alemania
Fil: Ferraz Mello, S.. Universidade de Sao Paulo; Brasil
Fil: Guenther, E.W.. Thüringer Landessternwarte; Alemania
Fil: Guillot, T.. Université Côte d’Azur; Francia
Fil: Grziwa, S.. Universitat zu Köln; Alemania
Fil: Hatzes, A.. Thüringer Landessternwarte; Alemania
Fil: Hébrard, G.. Université Pierre et Marie Curie; Francia
Fil: Mazeh, T.. Universitat Tel Aviv; Israel
Fil: Ollivier, M.. Institut D'astrophysique Spatiale; Francia. Université Pierre et Marie Curie; Francia
Fil: Parviainen, H.. University of Oxford; Reino Unido
Fil: Pätzold, M.. Universitat zu Köln; Alemania
Fil: Rauer, H.. Technishe Universitat Berlin; Alemania. Center for Astronomy and Astrophysics; Alemania
Fil: Rouan, D.. Université Pierre et Marie Curie; Francia
Fil: Santerne, A.. Aix Marseille Université; Francia
Fil: Schneider, J.. Centre National de la Recherche Scientifique. Observatoire de Paris. Laboratoire de L`univers Et Ses Theories; Francia