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Observations of exoplanet atmospheres have revealed the presence of cloudparticles in their atmospheres. 3D modelling of cloud formation in atmospheresof extrasolar planets coupled to the atmospheric dynamics has long been achallenge. We investigate the thermo-hydrodynamic properties of cloud formationprocesses in the atmospheres of hot Jupiter exoplanets. We simulate the dynamicatmosphere of HD 189733b with a 3D model that couples 3Dradiative-hydrodynamics with a kinetic, microphysical mineral cloud formationmodule designed for RHD/GCM exoplanet atmosphere simulations. Our simulationincludes the feedback effects of cloud advection and settling, gas phaseelement advection and depletion/replenishment and the radiative effects ofcloud opacity. We model the cloud particles as a mix of mineral materials whichchange in size and composition as they travel through atmosphericthermo-chemical environments. All local cloud properties such as numberdensity, grain size and material composition are time-dependently calculated.Gas phase element depletion as a result of cloud formation is included in themodel. In-situ \textit{effective medium theory} and Mie theory is applied tocalculate the wavelength dependent opacity of the cloud component. We present a3D cloud structure of a chemically complex, gaseous atmosphere of the hotJupiter HD 189733b. Mean cloud particle sizes are typically sub-micron(0.01-0.5 $\mu$m) at pressures less than 1 bar with hotter equatorial regionscontaining the smallest grains. Denser cloud structures occur near terminatorregions and deeper ($\sim$ 1 bar) atmospheric layers. Silicate materials suchas MgSiO$_{3}$[s] are found to be abundant at mid-high latitudes, whileTiO$_{2}$[s] and SiO$_{2}$[s] dominate the equatorial regions.

Dynamic mineral clouds on HD 189733b I. 3D RHD with kinetic, non-equilibrium cloud formation