Transmission Spectra of Three-dimensional Hot Jupiter Model Atmospheres

Astronomy and Astrophysics – Astronomy

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Scientific paper

We generate one-dimensional and three-dimensional model transmission spectra of the atmospheres of HD 209458b and HD 189733b. We also examine the effects of temperature, surface gravity, and metallicity for hot Jupiters, in general. We find that carbon dioxide absorption features at 4.4 and 15 μm are prominent in high metallicity planets, and are a clear metallicity indicator. The three-dimensional models of HD 209458b show that although TiO and VO gases may be abundant on the day side hemisphere, these abundances can be greatly reduced near the cooler limb of the planet. One-dimensional model spectra for HD 189733b enable us to constrain the altitude of a postulated haze layer responsible for Rayleigh scattering in the optical. Three dimensional model spectra for HD 189733b show differences in carbon chemical abundances, when comparing the leading and trailing hemispheres. When assuming thermochemical equilibrium, the cooler leading hemisphere will be methane dominated while the hotter trailing hemisphere will be carbon monoxide dominated. However, if vertical mixing and nonequilibrium chemistry is important, these differences are removed. It is possible that JWST will be able to probe the spatial variation of carbon chemistry for this planet. The comparisons of these three-dimensional model atmospheres with data serve as constraints on these dynamical models that complement the secondary eclipse and light curve data sets.

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