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

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

doi:10.1051/0004-6361/202450307

paper

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

arXiv:2412.10192 · doi:10.1051/0004-6361/202450307

Abstract

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 loss, the time of mantle solidification for TRAPPIST-1 e, f, and g can be significantly extended compared to a pure H $_{2}$ O evolution by up to 40 Myrs for albedo 0.75 and by up to 200 Mrys for albedo 0. The addition of CO $_{2}$ further results in a higher water content in the melt during the magma ocean stage. Our compositional model adjusted for the measured metallicity of TRAPPIST-1 yields for the dry inner planets (b, c, d) an iron fraction of 27 wt-%. For TRAPPIST-1 e, this iron fraction would be compatible with a (partly) desiccated evolution scenario and a CO $_{2}$ atmosphere with surface pressures of a few 100 bar. A comparative study between TRAPPIST-1 e and the inner planets may yield the most insights about formation and evolution scenarios.

arXiv comment36 pages, 28 figues, accepted by A&A 9/12/2024

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

Abstract

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From CO2​- to H2​O-dominated atmospheres and back -- How mixed outgassing changes the volatile distribution in magma oceans around M dwarf stars

Abstract

References in corpus (70)

Cited by in corpus (2)

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