Young M dwarfs flare activity model: Towards better exoplanetary atmospheric characterisation

TL;DR

This paper introduces the YMDF model, a physically motivated tool combining radiative-hydrodynamic simulations and electron beam physics to accurately reproduce the spectral and temporal evolution of flares on young M dwarfs, aiding exoplanet atmosphere studies.

Contribution

The paper presents the development and validation of the YMDF model, integrating RHD models with electron beam physics to better simulate stellar flare spectra and energetics.

Findings

YMDF model reproduces observed continuum rise in TESS and FUV-A bands.

Flare distributions from YMDF align with observed stellar data.

Model provides a foundation for studying flare impacts on exoplanet atmospheres.

Abstract

Context. Stellar flares can significantly influence the atmospheres and habitability of orbiting exoplanets, especially around young and active M dwarfs. Understanding the temporally and spectrally resolved activity of such stars is essential for assessing their impact on planetary environments. Aims. We aim to examine in detail state-of-the-art concepts of flare models to identify what is missing in our understanding of energy deposition during the flare event. By comparing synthetic and observed flare spectra, we seek to determine the modelling frameworks best suited to represent flare energetics and spectral far-ultraviolet features while providing a foundation for investigating flare impacts on exoplanet atmospheres. Methods. In this work, we built the Young M Dwarfs Flare (YMDF) model utilising the combination of radiative-hydrodynamic (RHD) stellar atmosphere models with a high and low-energy electron beam and corresponding synthetic observables. These models are based on physical principles and were validated with solar and stellar observations. Results. The newly developed YMDF model reproduces the observed continuum rise in both the TESS photometric band and the FUV-A spectral range. Furthermore, the flare distributions generated within this framework show consistency with those observed in our sample of stars. Conclusions. We have developed the YMDF model as a tool to reproduce the time-dependent spectra of flaring young M dwarfs, providing a physically motivated description of their spectral and temporal evolution during flare events.