Transiting exoplanets from the CoRoT space mission: XXI. CoRoT-19b: A low density planet orbiting an old inactive F9V-star

E. W. Guenther, R. F. Díaz, J. C. Gazzano, T. Mazeh, D. Rouan, N. Gibson, Sz Csizmadia, S. Aigrain, R. Alonso, J. M. Almenara, M. Auvergne, A. Baglin, P. Barge, A. S. Bonomo, P. Bordé, F. Bouchy, H. Bruntt, J. Cabrera, L. Carone, S. CarpanoC. Cavarroc, H. J. Deeg, M. Deleuil, S. Dreizler, R. Dvorak, A. Erikson, S. Ferraz-Mello, M. Fridlund, D. Gandolfi, M. Gillon, T. Guillot, A. Hatzes, M. Havel, G. Hébrard, E. Jehin, L. Jorda, H. Lammer, A. Léger, C. Moutou, L. Nortmann, M. Ollivier, A. Ofir, Th Pasternacki, M. Pätzold, H. Parviainen, D. Queloz, H. Rauer, B. Samuel, A. Santerne, J. Schneider, L. Tal-Or, B. Tingley, J. Weingrill, G. Wuchterl

Research output: Contribution to journalArticlepeer-review

Abstract

Context. Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. These measurements indicate that planets of similar mass can have very different radii. For low-density planets, it is generally assumed that they are inflated owing to their proximity to the host-star. To determine the causes of this inflation, it is necessary to obtain a statistically significant sample of planets with precisely measured masses and radii. Aims. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. Methods. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. Results. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M * = 1.21 ± 0.05 M and radius R * = 1.65 ± 0.04 R . The planet has a mass of M P = 1.11 ± 0.06 M Jup and radius of R P = 1.29 ± 0.03 R Jup. The resulting bulk density is only ρ = 0.71 ± 0.06 g cm -3, which is much lower than that for Jupiter. Conclusions. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a ≈30% larger radius.

Original languageEnglish
Article numberA136
JournalAstronomy and Astrophysics
Volume537
DOIs
StatePublished - 2012

Keywords

  • planetary systems
  • techniques: photometric
  • techniques: radial velocities
  • techniques: spectroscopic

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