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Clouds are an integral part of planetary atmospheres, with most planetshosting clouds. The understanding of not only the formation, but also thecomposition of clouds is crucial to the understanding of future observations.As observations of the planet's surface will remain very difficult, it isessential to link the observable high atmosphere gas and cloud composition tothe surface conditions. We present a fast and simple chemical equilibrium (eq.)model for the troposphere of rocky exoplanets, which is in chemical and phaseeq. with the crust. The hydrostatic eq. atmosphere is built from bottom to top.In each atmospheric layer chemical eq. is solved and all thermally stablecondensates are removed, depleting the atmosphere above in the effectedelements. These removed condensates build an upper limit for cloud formationand can be separated into high and low temperature condensates. The mostimportant cloud condensates for 1000K>T>400K are KCl, NaCl, FeS, FeS2, FeO,Fe2O3, Fe3O4. For T<400K H2O, C, NH3, NH4Cl, NH4SH are thermally stable. Foreven lower temperatures of T<150K CO2, CH4, NH3, H2S become stable. Theinclusion of clouds with trace abundances results in the thermal stability of atotal of 72 condensates for atmospheres with the different surface conditions(300K<T<1000K and p=1bar,100bar). The different cloud condensates are notindependent of each other, but follow sequences of condensation, which arerobust against changes in crust composition, surface pressure, and surfacetemperature. Independent of the existence of water as a crust condensate H2O isa thermally stable cloud condensate for all investigated elemental abundances.However, the water cloud base depends on the hydration level of the crust.Therefore, the detection of water condensates alone does not necessarily implystable water on the surface, even if the temperature could allow watercondensation.

The Atmospheres of Rocky Exoplanets II. Influence of surface composition on the diversity of cloud condensates