Curtis S Cooper

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'Hot Jupiter' extrasolar planets are expected to be tidally locked because they are close (<0.05 astronomical units, where 1 au is the average Sun-Earth distance) to their parent stars, resulting in permanent daysides and nightsides. By observing systems where the planet and star periodically eclipse each other, several groups have been able to estimate the(More)
We calculate the meteorology of the close-in transiting extrasolar planet HD 209458b using a global, three-dimensional atmospheric circulation model. Dynamics are driven by perpetual irradiation of one hemisphere of this tidally locked planet. The simulation predicts global temperature contrasts of ∼ 500 K at the photosphere and the development of a steady(More)
We present global, three-dimensional numerical simulations of the atmospheric circulation on HD209458b and HD189733b and calculate the infrared spectra and light curves predicted by these simulations, which we compare with available observations. Radiative heating/cooling is parameterized with a simplified Newtonian relaxation scheme. Our simulations(More)
We present a method that employs the secondary eclipse light curves of tran-siting extrasolar planets to probe the spatial variation of their thermal emission. This technique permits an observer to resolve the surface of the planet without the need to spatially resolve its central star. We evaluate the feasibility of this technique for the HD 209458 system(More)
Chemical equilibrium considerations suggest that, assuming solar elemental abundances, carbon on HD 209458b is sequestered primarily as carbon monoxide (CO) and methane (CH 4). The relative mole fractions of CO(g) and CH 4 (g) in chemical equilibrium are expected to vary greatly according to variations in local temperature and pressure. We show, however,(More)
Chemical equilibrium considerations suggest that, assuming solar elemental abundances, carbon on HD 209458b is sequestered primarily as carbon monoxide (CO) and methane (CH 4). The relative mole fractions of CO(g) and CH 4 (g) in chemical equilibrium are expected to vary greatly according to variations in local temperature and pressure. We show, however,(More)
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