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Title:
Photometrically Derived Masses and Radii of the Planet and Star in the TrES-2 System
Authors:
Barclay, Thomas; Huber, Daniel; Rowe, Jason F.; Fortney, Jonathan J.; Morley, Caroline V.; Quintana, Elisa V.; Fabrycky, Daniel C.; Barentsen, Geert; Bloemen, Steven; Christiansen, Jessie L.; Demory, Brice-Olivier; Fulton, Benjamin J.; Jenkins, Jon M.; Mullally, Fergal; Ragozzine, Darin; Seader, Shaun E.; Shporer, Avi; Tenenbaum, Peter; Thompson, Susan E.
Affiliation:
AA(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; Bay Area Environmental Research Institute, Inc., 560 Third Street West, Sonoma, CA 95476, USA), AB(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; NASA Postdoctoral Program Fellow.), AC(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AD(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA), AE(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA), AF(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AG(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA; Hubble Fellow.), AH(Armagh Observatory, College Hill, Armagh BT61 9DG, UK), AI(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, B-3001 Leuven, Belgium), AJ(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AK(Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA), AL(Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USA), AM(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AN(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AO(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AP(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AQ(Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USA; Department of Physics, Broida Hall, University of California, Santa Barbara, CA 93106, USA), AR(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA), AS(NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA ; SETI Institute, 189 Bernardo Avenue, Suite 100, Mountain View, CA 94043, USA)
Publication:
The Astrophysical Journal, Volume 761, Issue 1, article id. 53, 10 pp. (2012). (ApJ Homepage)
Publication Date:
12/2012
Origin:
IOP
Astronomy Keywords:
planets and satellites: individual: TrES-2b, stars: individual: TrES-2A, techniques: photometric
DOI:
10.1088/0004-637X/761/1/53
Bibliographic Code:
2012ApJ...761...53B

Abstract

We measure the mass and radius of the star and planet in the TrES-2 system using 2.7 years of observations by the Kepler spacecraft. The light curve shows evidence for ellipsoidal variations and Doppler beaming on a period consistent with the orbital period of the planet with amplitudes of 2.79+0.44 -0.62 and 3.44+0.32 -0.37 parts per million (ppm), respectively, and a difference between the dayside and the nightside planetary flux of 3.41+0.55 -0.82 ppm. We present an asteroseismic analysis of solar-like oscillations on TrES-2A which we use to calculate the stellar mass of 0.94 ± 0.05 M and radius of 0.95 ± 0.02 R . Using these stellar parameters, a transit model fit and the phase-curve variations, we determine the planetary radius of 1.162+0.020 -0.024 R Jup and derive a mass for TrES-2b from the photometry of 1.44 ± 0.21 M Jup. The ratio of the ellipsoidal variation to the Doppler beaming amplitudes agrees to better than 2σ with theoretical predications, while our measured planet mass and radius agree within 2σ of previously published values based on spectroscopic radial velocity measurements. We measure a geometric albedo of 0.0136+0.0022 -0.0033 and an occultation (secondary eclipse) depth of 6.5+1.7 -1.8 ppm which we combined with the day/night planetary flux ratio to model the atmosphere of TrES-2b. We find that an atmosphere model that contains a temperature inversion is strongly preferred. We hypothesize that the Kepler bandpass probes a significantly greater atmospheric depth on the night side relative to the day side.
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