Volatile atmospheres of lava worlds^★

¹ Laboratoire de Météorologie Dynamique, IPSL, CNRS, 4 Place Jussieu, 75252 Paris, France
e-mail: maximemaurice@protonmail.com
² Rice University, Earth, Environmental and Planetary Sciences Department, 6100 Main Street, MS 126, Houston, TX 77005, USA
³ Rice University, Mechanical Engineering Department, 6100 Main Street, MS 126, Houston, TX 77005, USA

Received: 17 August 2023
Accepted: 30 April 2024

Abstract

Context. A magma ocean (MO) is thought to be a ubiquitous stage in the early evolution of rocky planets and exoplanets. During the lifetime of the MO, exchanges between the interior and exterior envelopes of the planet are very efficient. In particular, volatile elements that initially are contained in the solid part of the planet can be released and form a secondary outgassed atmosphere.

Aims. We determine trends in the H–C–N–O–S composition and thickness of these secondary atmospheres for varying planetary sizes and MO extents, and the oxygen fugacity of MOs, which provides the main control for the atmospheric chemistry.

Methods. We used a model with coupled chemical gas-gas and silicate melt-gas equilibria and mass conservation to predict the composition of an atmosphere at equilibrium with the MO depending on the planet size and the extent and redox state of the MO. We used a self-consistent mass–radius model for the rocky core to inform the structure of the planet, which we combined with an atmosphere model to predict the transit radius of lava worlds.

Results. The resulting MOs have potential temperatures ranging from 1415 to 4229 K, and their outgassed atmospheres have total pressures from 3.3 to 768 bar. We find that MOs (especially the shallow ones) on small planets are generally more reduced, and are thus dominated by H₂-rich atmospheres (whose outgassing is strengthened at low planetary mass), while larger planets and deeper MOs vary from CO to CO₂–N₂–SO₂ atmospheres, with increasing $f_{{\mathrm{O}}_2}$. In the former case, the low molecular mass of the atmosphere combined with the low gravity of the planets yields a large vertical extension of the atmosphere, while in the latter cases, secondary outgassed atmospheres on super-Earths are likely significantly shrunk. Both N and C are largely outgassed regardless of the conditions, while the S and H outgassing is strongly dependent on the $f_{{\mathrm{O}}_2}$, as well as on the planetary mass and MO extent for the latter. We further use these results to assess how much a secondary outgassed atmosphere may alter the mass–radius relations of rocky exoplanets.