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3D atmosphere model results are used to comparatively study the kinetic,non-equilibrium cloud formation in the atmospheres of two example planetsguided by the giant gas planets HD209458b and HD189733b. Rather independentlyof hydrodynamic model differences, our cloud modelling suggests that bothplanets are covered in mineral clouds throughout the entire modelling domain.Both planets harbour chemically complex clouds that are made of mineralparticles that have a height-dependent material composition and size. Theremaining gas-phase element abundances strongly effects the molecularabundances of the atmosphere in the cloud forming regions. Hydrocarbon andcyanopolyyne molecules can be rather abundant in the inner, dense part of theatmospheres of HD189733b and HD209458b. No one value for metallicity and theC/O ratio can be used to describe an extrasolar planet. Our results concerningthe presence and location of water in relation to the clouds explain some ofthe observed differences between the two planets. In HD189733b, strong waterfeatures have been reported while such features appear less strong forHD209458b. By considering the location of the clouds in the two atmospheres, wesee that obscuring clouds exist high in the atmosphere of HD209458b, but muchdeeper in HD189733b. We further conclude that the (self-imposed) degeneracy ofcloud parameters in retrieval methods can only be lifted if the cloud formationprocesses are accurately modelled in contrast to prescribing them byindependent parameters.

The mineral clouds on HD 209458b and HD189733b