Chemical variation with altitude and longitude on exo-Neptunes: Predictions for Ariel phase-curve observations

Abstract

Using 2D thermal structure models and pseudo-2D chemical kinetics models, we explore how atmospheric temperatures and composition change as a function of altitude and longitude within the equatorial regions of close-in transiting Neptune-class exoplanets at different distances from their host stars. Our models predict that the day-night stratospheric temperature contrasts increase with increasing planetary effective temperatures T_eff; atmospheric composition also changes significantly with T_eff. Horizontal transport-induced quenching is very effective in our simulated exo-Neptune atmospheres, acting to homogenize the vertical profiles of species abundances with longitude at stratospheric pressures where infrared observations are sensitive. Our models have important implications for planetary emission observations as a function of orbital phase with the Ariel mission. Cooler solar-composition exo-Neptunes with T_eff = 500-700 K are predicted to have small variations in infrared emission spectra with orbital phase, making them less robust phase-curve targets for Ariel. Hot solar-composition exo-Neptunes with T_eff > 1300 K exhibit strong variations in infrared emission with orbital phase but are arguably less interesting from an atmospheric chemistry standpoint, with spectral signatures being dominated by a small number of species whose abundances are expected to be constant with longitude and consistent with thermochemical equilibrium. Solar-composition exo-Neptunes with T_eff = 900-1100 K reside in an interesting intermediate regime, with infrared phase curve variations being affected by both temperature and composition variations. This interesting intermediate regime shifts to smaller temperatures as atmospheric metallicity is increased, making cool higher-metallicity Neptune-class planets appropriate targets for Ariel phase-curve observations.