Carbon cycling and interior evolution of water-covered plate tectonics and stagnant lid planets

Abstract

Aims: The long-term carbon cycle for planets with a surface entirely covered by oceans works differently from that of the present-day Earth because inefficient erosion leads to a strong dependence of the weathering rate on the rate of volcanism. In this paper, we investigate the long-term carbon cycle for these planets throughout their evolution. Methods: We built box models of the long-term carbon cycle based on CO${}_2$ degassing, seafloor-weathering, metamorphic decarbonation, and ingassing and coupled them with thermal evolution models of stagnant lid and plate tectonics planets. Results: The assumed relationship between the seafloor-weathering rate and the atmospheric CO${}_2$ or the surface temperature strongly influences the climate evolution for both tectonic regimes. For a plate tectonics planet, the atmospheric CO${}_2$ partial pressure is characterised by an equilibrium between ingassing and degassing and depends on the temperature gradient in subduction zones affecting the stability of carbonates. For a stagnant lid planet, partial melting and degassing are always accompanied by decarbonation, such that the combined carbon content of the crust and atmosphere increases with time. Whereas the initial mantle temperature for plate tectonics planets only affects the early evolution, it influences the evolution of the surface temperature of stagnant lid planets for much longer. Conclusions: For both tectonic regimes, mantle cooling results in a decreasing atmospheric CO${}_2$ partial pressure. For a plate tectonics planet this is caused by an increasing fraction of subduction zones that avoid crustal decarbonation, and for stagnant lid planets this is caused by an increasing decarbonation depth. This mechanism may partly compensate for the increase of the surface temperature due to increasing solar luminosity with time and hereby contribute to keep planets habitable in the long-term.

References in corpus (7)

• Inevitability of Plate Tectonics on Super-Earths
• Geodynamics and Rate of Volcanism on Massive Earth-like Planets
• Whole planet coupling between climate, mantle, and core: Implications for the evolution of rocky planets
• The habitability of a stagnant-lid Earth
• Habitability of Earth-like stagnant lid planets: Climate evolution and recovery from snowball states
• The habitability of stagnant-lid Earths around dwarf stars
• Bifurcation in the growth of continental crust

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