Issue |
A&A
Volume 543, July 2012
|
|
---|---|---|
Article Number | L5 | |
Number of page(s) | 5 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201219533 | |
Published online | 29 June 2012 |
Letter to the Editor
Doppler tomography of transiting exoplanets: a prograde, low-inclined orbit for the hot Jupiter CoRoT-11b
1
Research and Scientific Support Department,
ESTEC/ESA, PO Box 299
2200 AG
Noordwijk,
The Netherlands
e-mail: davide.gandolfi@esa.int
2
School of Physics & Astronomy, University of St.
Andrews, North Haugh, St.
Andrews, Fife
KY16 9SS,
UK
3
McDonald Observatory, University of Texas at Austin,
Austin,
TX
78712,
USA
4
INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78,
95123
Catania,
Italy
5
Laboratoire d’Astrophysique de Marseille, CNRS &
University of Provence, 38 rue
Frédéric Joliot-Curie, 13388
Marseille Cedex 13,
France
6
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205
La Laguna,
Spain
7
Departamento de Astrofísica, Universidad de La
Laguna, 38206
La Laguna,
Spain
8
Thüringer Landessternwarte, Sternwarte 5, Tautenburg,
07778
Tautenburg,
Germany
Received:
3
May
2012
Accepted:
12
June
2012
We report the detection of the Doppler shadow of the transiting hot Jupiter CoRoT-11b. Our analysis is based on line-profile tomography of time-series, Keck/HIRES high-resolution spectra acquired during the transit of the planet. We measured a sky-projected, spin-orbit angle λ = 0.1° ± 2.6°, which is consistent with a very low-inclined orbit with respect to the stellar rotation axis. We refined the physical parameters of the system using a Markov chain Monte Carlo simultaneous fitting of the available photometric and spectroscopic data. An analysis of the tidal evolution of the system shows how the currently measured obliquity and its uncertainty translate into an initial absolute value of less than about 10° on the zero-age main sequence, for an expected average modified tidal quality factor of the star ⟨ Q '* ' ⟩ ≳ 4 × 106. This is indicative of an inward migration scenario that would not have perturbed the primordial low obliquity of CoRoT-11b. Taking into account the effective temperature and mass of the planet host star (Teff = 6440 K, M⋆ = 1.23 M⊙), the system can be considered a new telling exception to the recently proposed trend, according to which relatively hot and massive stars (Teff > 6250 K, M⋆ > 1.2 M⊙) seem to be preferentially orbited by hot Jupiters with high obliquity.
Key words: planet-star interactions / planet-disk interactions / planetary systems / binaries: eclipsing / stars: individual: CoRoT-11
© ESO, 2012
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