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Almost all planetary atmospheres are affected by disequilibrium chemicalprocesses. In this paper we introduce our recently developed Chemical KineticModel (\texttt{ChemKM}). We show that the results of our HD189733b model are ingood agreement with previously published results, except at $\mu$bar regime,where molecular diffusion and photochemistry are the dominant processes. Wethus recommend careful consideration of these processes when abundances at thetop of the atmosphere are desired. We also propose a new metric for aquantitative measure of quenching levels. By applying this metric, we find thatquenching pressure decreases with the effective temperature of planets, but italso varies significantly with other atmospheric parameters such as [Fe/H],log(g), and C/O. In addition, we find that the "Methane Valley", a regionbetween 800 and 1500K where above a certain C/O threshold value a greaterchance of CH$_4$ detection is expected, still exists after including thevertical mixing. The first robust CH$_4$ detection on an irradiated planet(HD102195b) places this object within this region; supporting our prediction.We also investigate the detectability of disequilibrium spectral fingerprintsby JWST, and suggest focusing on the targets with T$_{eff}$ between 1000 and1800K, orbiting around M-dwarfs, having low surface gravity but highmetallicity and a C/O ratio value around unity. Finally, constructing Spitzercolor-maps suggests that the main two color-populations are largely insensitiveto the vertical mixing. Therefore any deviation of observational points fromthese populations are likely due to the presence of clouds and notdisequilibrium processes. However, some cold planets (T$_{eff}<$900K) with verylow C/O ratios ($<$0.25) show significant deviations; making these planetsinteresting cases for further investigation.

From cold to hot irradiated gaseous exoplanets: Fingerprints of chemical disequilibrium in atmospheric spectra