Recent infrared spectroscopy of hot exoplanets is beginning to reveal their atmospheric composition. Deep within planetary atmosphere, the composition is controlled by thermochemical equilibrium. Photochemistry becomes higher in the atmosphere, at levels above ~1 bar. These two chemistries compete between ~1 and 10 bars hot-Jupiter-like atmospheres, depending on the strength of the eddy mixing and temperature. HD 189733b an excellent laboratory in which to study the consequences of chemistry of hot atmospheres. The spectra of HD 189733b contain signatures of CH_4, CO_2, CO, and H_2O. Here we identify the primary pathways that govern the abundances of CH_4, CO_2, CO, and H_2O in the cases of thermochemical chemistry, photochemistry, and their combination. Our results suggest that the disequilibrium can significantly enhance the abundances of these species above their thermochemical equilibrium , so some caution must be taken when assuming that an atmosphere is in strict thermochemical equilibrium.
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Line et al. (2010) studied this question.
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