Semi-Empirical Modeling of the Atmospheres of the M Dwarf Exoplanet Hosts GJ 832 and GJ 581

TL;DR

This study develops semi-empirical models of GJ 832 and GJ 581 to synthesize their spectra, aiding in understanding their EUV radiation environments crucial for exoplanet atmospheric studies.

Contribution

The paper introduces a radiative transfer code SSRPM with extensive atomic/molecular data to model M dwarf stars and synthesize their spectra, including EUV fluxes.

Findings

EUV fluxes agree with other reconstruction methods

Spectral energy distributions differ significantly in the EUV range

GJ 832 shows higher magnetic activity than GJ 581

Abstract

Stellar ultraviolet (UV) radiation drives photochemistry, and extreme-ultraviolet (EUV) radiation drives mass loss in exoplanet atmospheres. However, the UV flux is partly unobservable due to interstellar absorption, particularly in the EUV range (100--912 A). It is therefore necessary to reconstruct the unobservable spectra in order to characterize the radiation environment of exoplanets. In the present work, we use a radiative transfer code SSRPM to build one-dimensional semi-empirical models of two M dwarf exoplanet hosts, GJ 832 and GJ 581, and synthesize their spectra. SSRPM is equipped with an extensive atomic and molecular database and full-NLTE capabilities. We use observations in the visible, ultraviolet, and X-ray ranges to constrain atmospheric structures of the modeled stars. The synthesized integrated EUV fluxes are found to be in good agreement with other reconstruction techniques, but the spectral energy distributions (SEDs) disagree significantly across the EUV range. More than 2/3 of the EUV flux is formed above $10^5$ K. We find that the far ultraviolet (FUV) continuum contributes 42--54 % of the entire FUV flux between 1450--1700 A. The comparison of stellar structures of GJ 832 and GJ 581 suggests that GJ 832 is a more magnetically active star, which is corroborated by other activity indicators.