PHOTOMETRICALLY DERIVED MASSES AND RADII OF THE PLANET AND STAR IN THE TrES-2 SYSTEM

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 supe...

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Bibliographic Details
Published in:The Astrophysical journal 2012-12, Vol.761 (1), p.1-10
Main Authors: Barclay, Thomas, Huber, Daniel, Rowe, Jason F, tney, Jonathan J, Morley, Caroline V, Quintana, Elisa V, Fabrycky, Daniel C, BARENTSEN, GEERT, Bloemen, Steven, Christiansen, Jessie L
Format: Article
Language:English
Subjects:
ALBEDO
Amplitudes
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
DIAGRAMS
Doppler
Doppler effect
ECLIPSE
Flux
MASS
Mathematical models
Night
PHOTOMETRY
PLANETS
PROBES
RADIAL VELOCITY
SATELLITES
STARS
STELLAR ATMOSPHERES
TEMPERATURE INVERSIONS
VISIBLE RADIATION
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Summary: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 super(+0.44) sub(-0.62) and 3.44 super(+0.32) sub(-0.37) parts per million (ppm), respectively, and a difference between the dayside and the nightside planetary flux of 3.41 super(+0.55) sub(-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 + or - 0.05 M sub([middot in circle]) and radius of 0.95 + or - 0.02 R sub([middot in circle]). Using these stellar parameters, a transit model fit and the phase-curve variations, we determine the planetary radius of 1.162 super(+0.020) sub(-0.024) R sub(Jup) and derive a mass for TrES-2b from the photometry of 1.44 + or - 0.21 M sub(Jup). The ratio of the ellipsoidal variation to the Doppler beaming amplitudes agrees to better than 2[sigma] with theoretical predications, while our measured planet mass and radius agree within 2[sigma] of previously published values based on spectroscopic radial velocity measurements. We measure a geometric albedo of 0.0136 super(+0.0022) sub(-0.0033) and an occultation (secondary eclipse) depth of 6.5 super(+1.7) sub(-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.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/761/1/53