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On hot Jupiter exoplanets, strong horizontal and vertical winds shouldhomogenize the abundances of the important absorbers CH$_4$ and CO much fasterthan chemical reactions restore chemical equilibrium. This effect, typicallyneglected in general circulation models (GCMs), has been suggested asexplanation for discrepancies between observed infrared lightcurves and thosepredicted by GCMs: On the nightsides of several hot Jupiters, GCMs predictoutgoing fluxes that are too large, especially in the Spitzer 4.5 $\mu$m band.We modified the SPARC/MITgcm to include disequilibrium abundances of CH$_4$, COand H$_2$O by assuming that the CH$_4$/CO ratio is constant throughout thesimulation domain. We ran simulations of hot Jupiter HD 189733b with 8CH$_4$/CO ratios. In the more likely CO-dominated regime, we find temperaturechanges $\geq$50-100 K compared to the equilibrium chemistry case across largeregions. This effect is large enough to affect predicted emission spectra andshould thus be included in GCMs of hot Jupiters with equilibrium temperaturesbetween 600K and 1300K. We find that spectra in regions with strong methaneabsorption, including the Spitzer 3.6 and 8 $\mu$m bands, are strongly impactedby disequilibrium abundances. We expect chemical quenching to result in muchlarger nightside fluxes in the 3.6 $\mu$m band, in stark contrast toobservations. Meanwhile, we find almost no effect on predicted observations inthe 4.5 $\mu$m band, as the opacity changes due to CO and H$_2$O offset eachother. We thus conclude that disequilibrium carbon chemistry cannot explain theobserved low nightside fluxes in the 4.5 $\mu$m band.

astrophysical journal/the astrophysical journal

The Effect of 3D Transport-Induced Disequilibrium Carbon Chemistry on  the Atmospheric Structure and Phase Curves and Emission Spectra of Hot  Jupiter HD 189733b