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

M. Gillon, A. A. Lanotte, Travis S Barman, N. Miller, B. O. Demory, M. Deleuil, J. Montalbán, F. Bouchy, A. Collier Cameron, H. J. Deeg, J. J. Fortney, M. Fridlund, J. Harrington, P. Magain, C. Moutou, D. Queloz, H. Rauer, D. Rouan, J. Schneider

Research output: Contribution to journalArticle

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Abstract

We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm 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 μm. 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 (Mp = 3.47 ± 0.22 MJ , Rp = 1.466 ± 0.044 RJ ). 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 ω = -0.00291 ± 0.00063 where e is the orbital eccentricity and ω 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 Qs = 105-106, our modeling is able to explain the large radius of CoRoT-2b if Qp ≤ 105.5 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.

Original languageEnglish (US)
JournalAstronomy and Astrophysics
Volume511
Issue number1
DOIs
StatePublished - Feb 2010
Externally publishedYes

Fingerprint

thermal emission
planets
planet
orbitals
occultation
eccentricity
Roche limit
free atmosphere
temperature inversions
inversion layer
temperature inversion
optical measurement
night
ambiguity
young
cameras
time measurement
inversions
heating
wavelength

Keywords

  • Binaries: eclipsing
  • Planetary systems
  • Stars: individual: CoRoT-2
  • Techniques: photometric

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μ m * **. / Gillon, M.; Lanotte, A. A.; Barman, Travis S; Miller, N.; Demory, B. O.; Deleuil, M.; Montalbán, J.; Bouchy, F.; Collier Cameron, A.; Deeg, H. J.; Fortney, J. J.; Fridlund, M.; Harrington, J.; Magain, P.; Moutou, C.; Queloz, D.; Rauer, H.; Rouan, D.; Schneider, J.

In: Astronomy and Astrophysics, Vol. 511, No. 1, 02.2010.

Research output: Contribution to journalArticle

Gillon, M, Lanotte, AA, Barman, TS, Miller, N, Demory, BO, Deleuil, M, Montalbán, J, Bouchy, F, Collier Cameron, A, Deeg, HJ, Fortney, JJ, Fridlund, M, Harrington, J, Magain, P, Moutou, C, Queloz, D, Rauer, H, Rouan, D & Schneider, J 2010, 'The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μ m * **', Astronomy and Astrophysics, vol. 511, no. 1. https://doi.org/10.1051/0004-6361/200913507
Gillon, M. ; Lanotte, A. A. ; Barman, Travis S ; Miller, N. ; Demory, B. O. ; Deleuil, M. ; Montalbán, J. ; Bouchy, F. ; Collier Cameron, A. ; Deeg, H. J. ; Fortney, J. J. ; Fridlund, M. ; Harrington, J. ; Magain, P. ; Moutou, C. ; Queloz, D. ; Rauer, H. ; Rouan, D. ; Schneider, J. / The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μ m * **. In: Astronomy and Astrophysics. 2010 ; Vol. 511, No. 1.
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abstract = "We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm 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 μm. 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 (Mp = 3.47 ± 0.22 MJ , Rp = 1.466 ± 0.044 RJ ). 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 ω = -0.00291 ± 0.00063 where e is the orbital eccentricity and ω 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 Qs = 105-106, our modeling is able to explain the large radius of CoRoT-2b if Qp ≤ 105.5 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.",
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T1 - The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μ m * **

AU - Gillon, M.

AU - Lanotte, A. A.

AU - Barman, Travis S

AU - Miller, N.

AU - Demory, B. O.

AU - Deleuil, M.

AU - Montalbán, J.

AU - Bouchy, F.

AU - Collier Cameron, A.

AU - Deeg, H. J.

AU - Fortney, J. J.

AU - Fridlund, M.

AU - Harrington, J.

AU - Magain, P.

AU - Moutou, C.

AU - Queloz, D.

AU - Rauer, H.

AU - Rouan, D.

AU - Schneider, J.

PY - 2010/2

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N2 - We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm 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 μm. 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 (Mp = 3.47 ± 0.22 MJ , Rp = 1.466 ± 0.044 RJ ). 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 ω = -0.00291 ± 0.00063 where e is the orbital eccentricity and ω 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 Qs = 105-106, our modeling is able to explain the large radius of CoRoT-2b if Qp ≤ 105.5 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.

AB - We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm 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 μm. 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 (Mp = 3.47 ± 0.22 MJ , Rp = 1.466 ± 0.044 RJ ). 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 ω = -0.00291 ± 0.00063 where e is the orbital eccentricity and ω 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 Qs = 105-106, our modeling is able to explain the large radius of CoRoT-2b if Qp ≤ 105.5 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.

KW - Binaries: eclipsing

KW - Planetary systems

KW - Stars: individual: CoRoT-2

KW - Techniques: photometric

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