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Thermochemical models have been used in the past to constrain the deep oxygenabundance in the gas and ice giant planets from tropospheric CO spectroscopicmeasurements. Knowing the oxygen abundance of these planets is a key to betterunderstand their formation. These models have widely used dry and/or moistadiabats to extrapolate temperatures from the measured values in the uppertroposphere down to the level where the thermochemical equilibrium betweenH$_2$O and CO is established. The mean molecular mass gradient produced by thecondensation of H$_2$O stabilizes the atmosphere against convection and resultsin a vertical thermal profile and H$_2$O distribution that departssignificantly from previous estimates. We revisit O/H estimates using anatmospheric structure that accounts for the inhibition of the convection bycondensation. We use a thermochemical network and the latest observations of COin Uranus and Neptune to calculate the internal oxygen enrichment required tosatisfy both these new estimates of the thermal profile and the observations.We also present the current limitations of such modeling.

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Thermochemistry and vertical mixing in the tropospheres of Uranus and  Neptune: How convection inhibition can affect the derivation of deep oxygen  abundances