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Disequilibrium chemical processes have a large effect upon the spectra ofsubstellar objects. To study these effects, dynamical disequilibrium has beenparameterized using the quench and eddy diffusion approximations, but littlework has been done to explore how these approximations perform under realisticplanetary conditions in different dynamical regimes. As a first step inaddressing this problem, we study the localized, small scale convectivedynamics of planetary atmospheres by direct numerical simulation of fullycompressible hydrodynamics with reactive tracers using the Dedalus code. Usingpolytropically-stratified, plane parallel atmospheres in 2- and 3-D, we explorethe quenching behavior of different abstract chemical species as a function ofthe dynamical conditions of the atmosphere as parameterized by the Rayleighnumber. We find that in both 2- and 3-D, chemical species quench deeper thanwould be predicted based on simple mixing length arguments. Instead, it isnecessary to employ length scales based on the chemical equilibrium profile ofthe reacting species in order to predict quench points and perform chemicalkinetics modeling in 1-D. Based on the results of our simulations, we provide anew length scale, derived from the chemical scale height, which can be used toperform these calculations. This length scale is simple to calculate from knownchemical data and makes reasonable predictions for our dynamical simulations.

Convective dynamics and disequilibrium chemistry in the atmospheres of giant planets and brown dwarfs