Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d

Abstract Sub-Neptunes with substantial atmospheres may possess magma oceans in contact with the overlying gas, with chemical interactions between the atmosphere and magma playing an important role in shaping atmospheric composition. Early JWST observations have found high abundances of carbon- and oxygen-bearing molecules in a number of sub-Neptune atmospheres, which may result from processes including accretion of icy material at formation or magma–atmosphere interactions. Previous work examining the effects of magma–atmosphere interactions on sub-Neptunes has mostly been limited to studying conditions at the atmosphere–mantle boundary, without considering implications for the upper atmosphere, which is probed by spectroscopic observations. In this work, we present a modeling architecture to determine observable signatures of magma–atmosphere interactions. We combine an equilibrium chemistry code which models reactions between the core, mantle, and atmosphere with a radiative–convective model that determines the composition and structure of the observable upper atmosphere. We examine how different conditions at the atmosphere–mantle boundary and different core and mantle compositions impact the upper atmospheric composition. We compare our models to JWST NIRISS + NIRSpec observations of the sub-Neptune TOI-270 d, finding that our models can provide a good fit to the observed transmission spectrum with little fine-tuning. This suggests that magma–atmosphere interactions may be sufficient to explain the high abundances of molecules such as H 2 O, CH 4 , and CO 2 in sub-Neptune atmospheres, without additional accretion of icy material from the protoplanetary disk. Although other processes could lead to similar compositions, our work highlights the need to consider magma–atmosphere interactions when interpreting the observed atmospheric composition of a sub-Neptune.