Title

The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 mu m

Authors

Authors

M. Gillon; A. A. Lanotte; T. Barman; N. Miller; B. O. Demory; M. Deleuil; J. Montalban; F. Bouchy; A. C. Cameron; H. J. Deeg; J. J. Fortney; M. Fridlund; J. Harrington; P. Magain; C. Moutou; D. Queloz; H. Rauer; D. Rouan;J. Schneider

Comments

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Abbreviated Journal Title

Astron. Astrophys.

Keywords

binaries: eclipsing; planetary systems; stars: individual: CoRoT-2; techniques: photometric; STELLAR ATMOSPHERE MODELS; TRANSITING GIANT PLANETS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; MAIN-SEQUENCE STARS; LIGHT-CURVE PROJECT; LIMB-DARKENING LAW; EXTRASOLAR PLANET; TEMPERATURE; INVERSION; SECONDARY ECLIPSE; Astronomy & Astrophysics

Abstract

We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 mu m with the Spitzer Infrared Array Camera (IRAC). Our measured occultation depths are 0.510 +/- 0.042% at 4.5 and 0.41 +/- 0.11% at 8 mu m. In addition to the CoRoT optical measurements, these planet/star flux ratios indicate a poor heat distribution on the night side of the planet and agree better with an atmosphere free of temperature inversion layer. Still, such an inversion is not definitely ruled out by the observations and a larger wavelength coverage is required to remove the current ambiguity. Our global analysis of CoRoT, Spitzer, and ground-based data confirms the high mass and large size of the planet with slightly revised values (M(p) = 3.47 +/- 0.22 M(J), R(p) = 1.466 +/- 0.044 R(J)). We find a small but significant offset in the timing of the occultation when compared to a purely circular orbital solution, leading to e cos omega = -0.00291 +/- 0.00063 where e is the orbital eccentricity and omega is the argument of periastron. Constraining the age of the system to at most a few hundred Myr and assuming that the non-zero orbital eccentricity does not come from a third undetected body, we modeled the coupled orbital-tidal evolution of the system with various tidal Q values, core sizes, and initial orbital parameters. For Q(s)' = 10(5)-10(6), our modeling is able to explain the large radius of CoRoT-2b if Q(p)' <= 10(5.5) through a transient tidal circularization and corresponding planet tidal heating event. Under this model, the planet will reach its Roche limit within 20 Myr at most.

Journal Title

Astronomy & Astrophysics

Volume

511

Publication Date

1-1-2010

Document Type

Article

Language

English

First Page

11

WOS Identifier

WOS:000275752400030

ISSN

0004-6361

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