  Spectral features in the observed spectra of exoplanets depend on the
composition of their atmospheres. A good knowledge of the main atmospheric
processes that drive the chemical distribution is therefore essential to
interpret exoplanetary spectra. An atmosphere reaches chemical equilibrium if
the rates of the forward and backward chemical reactions converge to the same
value. However, there are atmospheric processes, such as atmospheric transport,
that destabilize this equilibrium. In this work we study the changes in
composition driven by a 3D wind field in WASP-43b using our Global Circulation
Model, THOR. Our model uses validated temperature- and pressure-dependent
chemical timescales that allow us to explore the disequilibrium chemistry of
CO, CO$_2$, H$_2$O and CH$_4$. In WASP-43b the formation of the equatorial jet
has an important impact in the chemical distribution of the different species
across the atmosphere. At low latitudes the chemistry is longitudinally
quenched, except for CO$_2$ at solar abundances. The polar vortexes have a
distinct chemical distribution since these are regions with lower temperature
and atmospheric mixing. Vertical and latitudinal mixing have a secondary impact
in the chemical transport. We determine graphically the effect of
disequilibrium on observed emission spectra. Our results do not show any
significant differences in the emission spectra between the equilibrium and
disequilibrium solutions for C/O = 0.5. However, if C/O is increased to 2.0,
differences in the spectra due to the disequilibrium chemistry of CH$_4$ become
non-negligible. In some spectral ranges the emission spectra can have more than
15$\%$ departures from the equilibrium solution.
