J/A+A/511/A3ivo://CDS.VizieR/J/A+A/511/A3doi:10.26093/cds/vizier.35110003CDSGillon M.Lanotte A.A.Barman T.Miller N.Demory B.-O.Deleuil M.,Montalban 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.2017-06-30T05:48:19Z2010-03-15T07:42:10ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.freclipsing-binary-starssolar-system-planetsapparent-magnitudeWe report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8um 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 8um. 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+/-0.22M_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 20Myr at most.2010A&A...511A...3Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/511/A3CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/corot : CoRoT observation log Release 4 (CoRoT, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/511/A3https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/511/A3http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/511/A3https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/511/A3https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/511/A3http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/511/A3GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/511/A3/forszVLT/FORS2 photometric time seriesAirmassAirmassobs.airMassdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian Datedtime.epochdoubleFluxFlux in z-bandphot.mag;em.opt.Idoublee_FluxError on fluxstat.error;phot.fluxdoubleJ/A+A/511/A3/iracch2IRAC 4.5um photometric time seriesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian Datedtime.epochdoubleFluxFlux at 4.5umphot.mag;em.IR.4-8umdoublee_FluxError on Fluxstat.error;phot.fluxdoubleXposX-position of the PSF centroid on the chippixpos.cartesian.x;instr.detdoubleYposY-position of the PSF centroid on the chippixpos.cartesian.y;instr.detdoubleJ/A+A/511/A3/iracch4IRAC 8um photometric time seriesFluxFlux at 8umphot.flux.density;em.IR.8-15umdoublee_FluxError on Fluxstat.error;phot.fluxdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian Datedtime.epochdouble