TY - JOUR
T1 - A theoretical interpretation of the measurements of the secondary eclipses of TrES-1 and HD 209458b
AU - Burrows, A.
AU - Hubeny, I.
AU - Sudarsky, D.
N1 - Funding Information:
We thank Christopher Sharp, Bill Hubbard, and Drew Mil-som for useful discussions during the course of this investigation and Dave Charbonneau for an advanced look at the TrES-1 secondary eclipse data. This study was supported in part by NASA grants NNG04GL22G and NAG5-13775. This material is based on work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement CAN-02-OSS-02 issued through the Office of Space Science.
PY - 2005/6/1
Y1 - 2005/6/1
N2 - We calculate the planet-to-star flux density ratios as a function of wavelength from 0.5 to 25 μm for the transiting extrasolar giant planets TrES-1 and HD 209458h and compare them with the recent Spitzer/IRAC-MIPS secondary eclipse data in the 4.5, 8.0, and 24 μm bands. With only three data points and generic calibration issues, detailed conclusions are difficult, but inferences regarding atmospheric composition, temperature, and global circulation can be made. Our models reproduce the observations reasonably well, but not perfectly, and we speculate on the theoretical consequences of variations around our baseline models. One preliminary conclusion is that we may be seeing in the data indications that the day side of a close-in extrasolar giant planet is brighter in the mid-infrared than its night side, unlike Jupiter and Saturn. This correspondence will be further tested when the data anticipated in other Spitzer bands are acquired, and we make predictions for what those data may show.
AB - We calculate the planet-to-star flux density ratios as a function of wavelength from 0.5 to 25 μm for the transiting extrasolar giant planets TrES-1 and HD 209458h and compare them with the recent Spitzer/IRAC-MIPS secondary eclipse data in the 4.5, 8.0, and 24 μm bands. With only three data points and generic calibration issues, detailed conclusions are difficult, but inferences regarding atmospheric composition, temperature, and global circulation can be made. Our models reproduce the observations reasonably well, but not perfectly, and we speculate on the theoretical consequences of variations around our baseline models. One preliminary conclusion is that we may be seeing in the data indications that the day side of a close-in extrasolar giant planet is brighter in the mid-infrared than its night side, unlike Jupiter and Saturn. This correspondence will be further tested when the data anticipated in other Spitzer bands are acquired, and we make predictions for what those data may show.
KW - Planetary systems -
KW - Planets and satellites: general -
KW - Stars: individual (HD 209458, TrES-1)
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U2 - 10.1086/431242
DO - 10.1086/431242
M3 - Review article
AN - SCOPUS:22544482981
SN - 0004-637X
VL - 625
SP - L135-L138
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -