# Analyzing Atmospheric Temperature Profiles and Spectra of M dwarf Rocky Planets

## TL;DR

This paper models atmospheres of three M-dwarf rocky exoplanets to predict their spectra and temperature profiles, aiding future JWST observations for atmospheric characterization.

## Contribution

It introduces detailed atmospheric models for three specific M-dwarf planets considering different compositions, highlighting the effects of stellar irradiation and opacity on spectra.

## Key findings

- Temperature inversions are common in cool M-dwarf planets due to strong absorption.
- Pure CO2 atmospheres are cooler and more reflective than H2O or solar-like compositions.
- JWST can potentially distinguish between different atmospheric compositions of these planets.

## Abstract

The James Webb Space Telescope (JWST) will open up the possibility of comprehensively measuring the emission spectra of rocky exoplanets orbiting M dwarfs to detect and characterize their atmospheres. In preparation for this opportunity, we present model atmospheres for three M-dwarf planets particularly amenable to secondary eclipse spectroscopy -- TRAPPIST-1b, GJ 1132b, and LHS 3844b. Using three limiting cases of candidate atmospheric compositions (pure H2O, pure CO2 and solar abundances) we calculate temperature-pressure profiles and emission and reflection spectra in radiative-convective equilibrium, including the effects of a solid surface. We find that the atmospheric radiative transfer is significantly influenced by the cool M-star irradiation; H2O and CO2 absorption bands in the near-infrared are strong enough to absorb a sizeable fraction of the incoming stellar light at low pressures, which leads to temperature inversions in the upper atmosphere. The non-gray band structure of gaseous opacities in the infrared is hereby an important factor. Opacity windows are muted at higher atmospheric temperatures, so we expect temperature inversions to be common only for sufficiently cool planets. We also find that pure CO2 atmospheres exhibit lower overall temperatures and stronger reflection spectra compared to models of the other two compositions. We estimate that for GJ 1132b and LHS 3844b we should be able to distinguish between different atmospheric compositions with JWST. The emission lines from the predicted temperature inversions are currently hard to measure, but high resolution spectroscopy with future Extremely Large Telescopes may be able to detect them.