  Almost all planetary atmospheres are affected by disequilibrium chemical
processes. In this paper we introduce our recently developed Chemical Kinetic
Model (\texttt{ChemKM}). We show that the results of our HD189733b model are in
good agreement with previously published results, except at $\mu$bar regime,
where molecular diffusion and photochemistry are the dominant processes. We
thus recommend careful consideration of these processes when abundances at the
top of the atmosphere are desired. We also propose a new metric for a
quantitative measure of quenching levels. By applying this metric, we find that
quenching pressure decreases with the effective temperature of planets, but it
also varies significantly with other atmospheric parameters such as [Fe/H],
log(g), and C/O. In addition, we find that the "Methane Valley", a region
between 800 and 1500K where above a certain C/O threshold value a greater
chance of CH$_4$ detection is expected, still exists after including the
vertical 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 fingerprints
by JWST, and suggest focusing on the targets with T$_{eff}$ between 1000 and
1800K, orbiting around M-dwarfs, having low surface gravity but high
metallicity and a C/O ratio value around unity. Finally, constructing Spitzer
color-maps suggests that the main two color-populations are largely insensitive
to the vertical mixing. Therefore any deviation of observational points from
these populations are likely due to the presence of clouds and not
disequilibrium processes. However, some cold planets (T$_{eff}<$900K) with very
low C/O ratios ($<$0.25) show significant deviations; making these planets
interesting cases for further investigation.
