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The ongoing discovery of terrestrial exoplanets accentuates the importance ofstudying planetary evolution for a wide range of initial conditions. We performthermal evolution simulations for generic terrestrial planets with massesranging from that of Mars to 10 Earth-masses in the stagnant-lid regime, themost natural mode of convection with strongly temperature- dependent viscosity.Given considerable uncertainty surrounding the dependency of mantle rheology onpressure, we choose to focus on the end-member case of pressure-independentpotential viscosity, where viscosity does not change with depth along anadiabatic temperature gradient. We employ principal component analysis andlinear regression to capture the first-order systematics of possibleevolutionary scenarios from a large number of simulation runs. With increasedplanetary mass, crustal thickness and the degree of mantle processing are bothpredicted to decrease, and such size effects can also be derived with simplescaling analyses. The likelihood of plate tectonics is quantified using amantle rheology that takes into account both ductile and brittle deformationmechanisms. Confirming earlier scaling analyses, the effects of lithospherehydration dominate the effects of planetary mass. The possibility ofbasalt-eclogite phase transition in the planetary crust is found to increasewith planetary mass, and we suggest that massive terrestrial planets may escapethe stagnant-lid regime through the formation of a self-destabilizing denseeclogite layer.

Terrestrial Planet Evolution in the Stagnant-Lid Regime: Size Effects and the Formation of Self-Destabilizing Crust