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Little is known about the interaction between atmospheres and crusts ofexoplanets so far, but future space missions and ground-based instruments areexpected to detect molecular features in the spectra of hot rocky exoplanets.We aim to understand the composition of the gas in an exoplanet atmospherewhich is in equilibrium with a planetary crust. Methods. The molecularcomposition of the gas above a surface made of a mixture of solid and liquidmaterials is determined by assuming phase equilibrium for given pressure,temperature and element abundances. We study total element abundances thatrepresent different parts of the Earth's crust (Continental Crust, BulkSilicate Earth, Mid Oceanic Ridge Basalt), CI chondrites and abundancesmeasured in polluted white dwarfs. For temperatures between 600K and 3500K, thenear-crust atmospheres of all considered total element abundances are mainlycomposed of H2O, CO2, SO2 and in some cases of O2 and H2. For temperatures500K, only N2-rich or CH4-rich atmospheres remain. For 3500K, the atmosphericgas is mainly composed of atoms (O, Na, Mg, Fe), metal oxides (SiO, NaO, MgO,CaO, AlO, FeO) and some metal hydroxides (KOH, NaOH). The inclusion ofphyllosilicates as potential condensed species is crucial for lowertemperatures, as they can remove water from the gas phase below about 700K andinhibit the presence of liquid water. Measurements of the atmosphericcomposition could, in principle, characterise the rock composition of exoplanetcrusts. H2O, O2 and CH4 are natural products from the outgassing of differentkinds of rocks that had time to equilibrate. These are discussed as biomarkers,but do emerge naturally as result of the thermodynamic interaction betweencrust and atmosphere. Only the simultaneous detection of all three moleculesmight be a sufficient biosignature, as it is inconsistent with chemicalequilibrium.

The Atmospheres of Rocky Exoplanets I. Outgassing of Common Rock and the Stability of Liquid Water