  Transport-induced quenching in hot Jupiter atmospheres is a process that
determines the boundary between the part of the atmosphere at chemical
equilibrium and the part of the atmosphere at thermochemical (but not
photothermochemical) disequilibrium. The location of this boundary, the quench
level, depends on the interplay between the dynamical and chemical timescales
in the atmosphere, with quenching occurring when these timescales are equal. We
explore the sensitivity of the quench level position to an increase in the
planet's atmospheric metallicity using aerosol-free 3D GCM simulations of a hot
Jupiter WASP-96b. We find that the temperature increase at pressures of
$\sim$$10^{4}-10^{7}$ Pa that occurs when metallicity is increased could shift
the position of the quench level to pressures dominated by the jet, and cause
an equatorial depletion of $CH_4$, $NH_3$ and $HCN$. We discuss how such a
depletion affects the planet's transmission spectrum, and how the analysis of
the evening-morning limb asymmetries, especially within $\sim3-5 {\mu}m$, could
help distinguish atmospheres of different metallicities that are at chemical
equilibrium from those with the upper layers at thermochemical disequilibrium.
