Inferring Shallow Surfaces on sub-Neptune Exoplanets with JWST

TL;DR

This study explores how trace gases like NH₃, HCN, and CH₃OH in sub-Neptune exoplanet atmospheres can indicate the presence of shallow surfaces, using photochemical modeling relevant for JWST observations.

Contribution

It provides detailed analysis of nitrogen conversion timescales and identifies methanol as a robust proxy for shallow surfaces on sub-Neptunes.

Findings

NH₃ conversion timescale ~1 million years

Methanol (CH₃OH) is a reliable surface proxy

NH₃ and CH₃OH are key indicators for JWST observations

Abstract

Planets smaller than Neptune and larger than Earth make up the majority of the discovered exoplanets. Those with H$_2$-rich atmospheres are prime targets for atmospheric characterization. The transition between the two main classes, super-Earths and sub-Neptunes, is not clearly understood as the rocky surface is likely not accessible to observations. Tracking several trace gases (specifically the loss of ammonia (NH$_3$) and hydrogen cyanide (HCN)) has been proposed as a proxy for the presence of a shallow surface. In this work, we revisit the proposed mechanism of nitrogen conversion in detail and find its timescale on the order of a million years. NH$_3$ exhibits dual paths converting to N$_2$ or HCN, depending on the UV radiation of the star and the stage of the system. In addition, methanol (CH$_3$OH) is identified as a robust and complementary proxy for a shallow surface. We follow the fiducial example of K2-18b with a 2D photochemical model (VULCAN) on an equatorial plane. We find a fairly uniform composition distribution below 0.1 mbar controlled by the dayside, as a result of slow chemical evolution. NH$_3$ and CH$_3$OH are concluded to be the most unambiguous proxies to infer surfaces on sub-Neptunes in the era of the James Webb Space Telescope (JWST).