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The oxidation of rocky planet surfaces and atmospheres, which arises from thetwin forces of stellar nucleosynthesis and gravitational differentiation, is auniversal process of key importance to habitability and exoplanet biosignaturedetection. Here we take a generalized approach to this phenomenon. Using asingle parameter to describe redox state, we model the evolution of terrestrialplanets around nearby M-stars and the Sun. Our model includes atmosphericphotochemistry, diffusion and escape, line-by-line climate calculations andinterior thermodynamics and chemistry. In most cases we find abioticatmospheric O2 buildup around M-stars during the pre-main sequence phase to bemuch less than calculated previously, because the planet's magma ocean absorbsmost oxygen liberated from H2O photolysis. However, loss of non-condensingatmospheric gases after the mantle solidifies remains a significant potentialroute to abiotic atmospheric O2 subsequently. In all cases, we predict thatexoplanets that receive lower stellar fluxes, such as LHS1140b and TRAPPIST-1fand g, have the lowest probability of abiotic O2 buildup and hence may be themost interesting targets for future searches for biogenic O2. Key remaininguncertainties can be minimized in future by comparing our predictions for theatmospheres of hot, sterile exoplanets such as GJ1132b and TRAPPIST-1b and --cwith observations.

Redox evolution via gravitational differentiation on low mass planets: implications for abiotic oxygen, water loss and habitability