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We measure the mass and radius of the star and planet in the TrES-2 systemusing 2.7 years of observations by the Kepler spacecraft. The light curve showsevidence for ellipsoidal variations and Doppler beaming on a period consistentwith the orbital period of the planet with amplitudes of 2.79+0.44-0.62 and3.44+0.32-0.37 parts per million (ppm) respectively, and a difference betweenthe day and night side planetary flux of 3.41+0.55-0.82 ppm. We present anasteroseismic analysis of solar-like oscillations on TrES-2A which we use tocalculate the stellar mass of 0.94+/-0.05 MSun and radius of 0.95+/-0.02 RSun.Using these stellar parameters, a transit model fit and the phase curvevariations, we determine the planetary radius of 1.162+0.020-0.024 RJup andderive a mass for TrES-2b from the photometry of 1.44+/-0.21 MJup. The ratio ofthe ellipsoidal variation to the Doppler beaming amplitudes agrees to betterthan 2{\sigma} with theoretical predications, while our measured planet massand radius agree within 2-{\sigma} of previously published values based onspectroscopic radial velocity measurements. We measure a geometric albedo of0.0136+0.0022-0.0033 and an occultation (secondary eclipse) depth of6.5+1.7-1.8 ppm which we combined with the day/night planetary flux ratio tomodel the atmosphere of TReS-2b. We find an atmosphere model that contains atemperature inversion is strongly preferred. We hypothesize that the Keplerbandpass probes a significantly greater atmospheric depth on the night siderelative to the day side.

Photometrically derived masses and radii of the planet and star in the TrES-2 system