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Disequilibrium species have been used previously to probe the deep waterabundances and the eddy diffusion coefficient for giant planets. In this paper,we present a diffusion-kinetics code that predicts the abundances ofdisequilibrium species in the tropospheres of Jupiter and Saturn with updatedthermodynamic and kinetic data. The dependence on the deep water abundance andthe eddy diffusion coefficient is investigated. We quantified the disagreementsin CO kinetics that comes from using different reaction networks and identifiedC$_2$H$_6$ as a useful tracer for the eddy diffusion coefficient. We firstapply a H/P/O reaction network to Jupiter and Saturn's atmospheres and suggesta new PH$_3$ destruction pathway. New chemical pathways for SiH$_4$ and GeH$_4$destruction are also suggested, and another AsH$_3$ destruction pathway isinvestigated thanks to new thermodynamic and kinetic data. These new modelsshould enhance the interpretation of the measurement of disequilibrium speciesby JIRAM on board Juno and allow disentangling between methods for constrainingthe Saturn's deep water abundance with the Saturn entry probes envisaged byNASA or ESA.

Modeling the disequilibrium species for Jupiter and Saturn: Implications for Juno and Saturn entry probe