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We present a study of the effect of wind-driven advection on the chemicalcomposition of hot Jupiter atmospheres using a fully-consistent 3Dhydrodynamics, chemistry and radiative transfer code, the Met Office UnifiedModel (UM). Chemical modelling of exoplanet atmospheres has primarily beenrestricted to 1D models that cannot account for 3D dynamical processes. In thiswork we couple a chemical relaxation scheme to the UM to account for thechemical interconversion of methane and carbon monoxide. This is doneconsistently with the radiative transfer meaning that departures from chemicalequilibrium are included in the heating rates (and emission) and hence completethe feedback between the dynamics, thermal structure and chemical composition.In this letter we simulate the well studied atmosphere of HD~209458b. We findthat the combined effect of horizontal and vertical advection leads to anincrease in the methane abundance by several orders of magnitude; directlyopposite to the trend found in previous works. Our results demonstrate the needto include 3D effects when considering the chemistry of hot Jupiteratmospheres. We calculate transmission and emission spectra, as well as theemission phase curve, from our simulations. We conclude that gas-phasenon-equilibrium chemistry is unlikely to explain the model-observationdiscrepancy in the 4.5\,{\textmu m} {\it Spitzer}/IRAC channel. However, wehighlight other spectral regions, observable with the James Webb SpaceTelescope, where signatures of wind-driven chemistry are more prominant.

Observable signatures of wind--driven chemistry with a fully consistent three dimensional radiative hydrodynamics model of HD 209458b