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

Journal Article · Mon Dec 10 00:00:00 EST 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/761/1/53· OSTI ID:22140040

Barclay, Thomas; Huber, Daniel; Rowe, Jason F.; Quintana, Elisa V.; Christiansen, Jessie L.; Jenkins, Jon M.; Mullally, Fergal; Seader, Shaun E.; Tenenbaum, Peter; Thompson, Susan E. ^[1]; Fortney, Jonathan J.; Morley, Caroline V.; Fabrycky, Daniel C. ^[2]; Barentsen, Geert ^[3]; Bloemen, Steven ^[4]; Demory, Brice-Olivier ^[5]; Fulton, Benjamin J.; Shporer, Avi ^[6]; Ragozzine, Darin ^[7]

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1. NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035 (United States)
2. Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States)
3. Armagh Observatory, College Hill, Armagh BT61 9DG (United Kingdom)
4. Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, B-3001 Leuven (Belgium)
5. Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139 (United States)
6. Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117 (United States)
7. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

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{sup +0.44}{sub -0.62} and 3.44{sup +0.32}{sub -0.37} parts per million (ppm), respectively, and a difference between the dayside and the nightside planetary flux of 3.41{sup +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 {+-} 0.05 M{sub Sun} and radius of 0.95 {+-} 0.02 R{sub Sun }. Using these stellar parameters, a transit model fit and the phase-curve variations, we determine the planetary radius of 1.162{sup +0.020}{sub -0.024} R{sub Jup} and derive a mass for TrES-2b from the photometry of 1.44 {+-} 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{sup +0.0022}{sub -0.0033} and an occultation (secondary eclipse) depth of 6.5{sup +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.

• OSTI ID: 22140040
• Journal Information: Astrophysical Journal, Vol. 761, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ALBEDO
ASTRONOMY
ASTROPHYSICS
DIAGRAMS
ECLIPSE
MASS
PHOTOMETRY
PLANETS
PROBES
RADIAL VELOCITY
SATELLITES
STARS
STELLAR ATMOSPHERES
TEMPERATURE INVERSIONS
VISIBLE RADIATION