Observability of signatures of transport-induced chemistry in clear atmospheres of hot gas giant exoplanets

Transport-induced quenching, i.e., the homogenisation of chemical abundances by atmospheric advection, is thought to occur in atmospheres hot gas giant exoplanets. While some numerical modelling this process exists, three-dimensional nature transport-induced chemistry underexplored. Here we present results 3D cloud- and haze-free simulations HAT-P-11b, HD 189733b, 209458b, WASP-17b including coupled hydrodynamics, radiative transfer chemistry. Our were performed with two schemes: a kinetics scheme, which capable capturing simpler, more widely used equilibrium scheme. We find that quenching predicted all planets our sample; however, extent it affects their synthetic spectra phase curves varies from planet planet. This implies there "sweet spot" for observability signatures controlled interplay between dynamics