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From CO$ 2$- to H$ 2$O-dominated atmospheres and back -- How mixed outgassing changes the volatile distribution in magma oceans around M dwarf stars by Carone, Ludmila; Barnes, Rory; Noack, Lena; Chubb, Katy L.; Barth, Patrick; Bitsch, Bertram; Thamm, Alexander; Balduin, Alexander; Garcia, Rodolfo; Helling, Christiane is a scholarly article available to read on EtoBox.

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We investigate the impact of CO$_2$ on TRAPPIST-1 e, f and g during the magma ocean stage. These potentially habitable rocky planets are currently the most accessible for astronomical observations. A constraint on the volatile budget during the magma ocean stage is a link to planet formation and also needed to judge their habitability. We perform simulations with 1-100 terrestrial oceans (TO) of H$_2$O with and without CO$_2$ and for albedos 0 and 0.75. The CO$_2$ mass is scaled with initial H$_2$O by a constant factor between 0.1 and 1. The magma ocean state of rocky planets begins with a CO$_2$-dominated atmosphere but can evolve into a H$_2$O dominated state, depending on initial conditions. For less than 10 TO initial H$_2$O, the atmosphere tends to desiccate and the evolution may end with a CO$_2$ dominated atmosphere. Otherwise, the final state is a thick (>1000 bar) H$_2$O-CO$_2$ atmosphere. Complete atmosphere desiccation with less than 10 TO initial H$_2$O can be significantly delayed for TRAPPIST-1e and f, when H$_2$O has to diffuse through a CO$_2$ atmosphere to reach the upper atmosphere, where XUV photolysis occurs. As a consequence of CO$_2$ diffusion-limited water lo

Author

Carone, Ludmila; Barnes, Rory; Noack, Lena; Chubb, Katy L.; Barth, Patrick; Bitsch, Bertram; Thamm, Alexander; Balduin, Alexander; Garcia, Rodolfo; Helling, Christiane

Published

2024

Language

EN