Abstract
We have created a general methodology for calculating the wavelength-dependent light curves of close-in extrasolar giant planets (EGPs) as they traverse their orbits. Focusing on the transiting EGPs HD 18973 3b, TrES-1, and HD 209458h, we calculate planet/star flux ratios during secondary eclipse and compare them with the Spitzer data points obtained so far in the mid-infrared. We introduce a simple parameterization for the redistribution of heat to the planet's night side, derive constraints on this parameter (P n), and provide a general set of predictions for planet/star contrast ratios as a function of wavelength, model, and phase. Moreover, we calculate average dayside and nightside atmospheric temperature/pressure profiles for each transiting planet/Pn pair with which existing and anticipated Spitzer data can be used to probe the atmospheric thermal structure of severely irradiated EGPs. We find that the baseline models do a good job of fitting the current secondary eclipse data set, but that the Spitzer error bars are not yet small enough to discriminate cleanly among all the various possibilities.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 1140-1149 |
| Number of pages | 10 |
| Journal | Astrophysical Journal |
| Volume | 650 |
| Issue number | 2 I |
| DOIs | |
| State | Published - Oct 20 2006 |
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Keywords
- Planetary systems
- Planets and satellites: general
- Stars: individual (TrES-1, HD 209458, HD 189733)
ASJC Scopus subject areas
- Space and Planetary Science
Cite this
Theory for the secondary eclipse fluxes, spectra, atmospheres, and light curves of transiting extrasolar giant planets. / Burrows, A.; Sudarsky, D.; Hubeny, Ivan -.
In: Astrophysical Journal, Vol. 650, No. 2 I, 20.10.2006, p. 1140-1149.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Theory for the secondary eclipse fluxes, spectra, atmospheres, and light curves of transiting extrasolar giant planets
AU - Burrows, A.
AU - Sudarsky, D.
AU - Hubeny, Ivan -
PY - 2006/10/20
Y1 - 2006/10/20
N2 - We have created a general methodology for calculating the wavelength-dependent light curves of close-in extrasolar giant planets (EGPs) as they traverse their orbits. Focusing on the transiting EGPs HD 18973 3b, TrES-1, and HD 209458h, we calculate planet/star flux ratios during secondary eclipse and compare them with the Spitzer data points obtained so far in the mid-infrared. We introduce a simple parameterization for the redistribution of heat to the planet's night side, derive constraints on this parameter (P n), and provide a general set of predictions for planet/star contrast ratios as a function of wavelength, model, and phase. Moreover, we calculate average dayside and nightside atmospheric temperature/pressure profiles for each transiting planet/Pn pair with which existing and anticipated Spitzer data can be used to probe the atmospheric thermal structure of severely irradiated EGPs. We find that the baseline models do a good job of fitting the current secondary eclipse data set, but that the Spitzer error bars are not yet small enough to discriminate cleanly among all the various possibilities.
AB - We have created a general methodology for calculating the wavelength-dependent light curves of close-in extrasolar giant planets (EGPs) as they traverse their orbits. Focusing on the transiting EGPs HD 18973 3b, TrES-1, and HD 209458h, we calculate planet/star flux ratios during secondary eclipse and compare them with the Spitzer data points obtained so far in the mid-infrared. We introduce a simple parameterization for the redistribution of heat to the planet's night side, derive constraints on this parameter (P n), and provide a general set of predictions for planet/star contrast ratios as a function of wavelength, model, and phase. Moreover, we calculate average dayside and nightside atmospheric temperature/pressure profiles for each transiting planet/Pn pair with which existing and anticipated Spitzer data can be used to probe the atmospheric thermal structure of severely irradiated EGPs. We find that the baseline models do a good job of fitting the current secondary eclipse data set, but that the Spitzer error bars are not yet small enough to discriminate cleanly among all the various possibilities.
KW - Planetary systems
KW - Planets and satellites: general
KW - Stars: individual (TrES-1, HD 209458, HD 189733)
UR - http://www.scopus.com/inward/record.url?scp=33845256672&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=33845256672&partnerID=8YFLogxK
U2 - 10.1086/507269
DO - 10.1086/507269
M3 - Article
AN - SCOPUS:33845256672
VL - 650
SP - 1140
EP - 1149
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2 I
ER -