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 .