Three-dimensional simulations of near-surface convection in main-sequence stars

Context. The near-surface layers of cool main-sequence stars are structured by convective flows, which are overshooting into the atmosphere. The flows and the associated spatio-temporal variations of density and temperature affect spectral line profiles and thus have an impact on estimates of stellar properties such as effective temperature, gravitational acceleration, and abundances. Aims. We aim at identifying distinctive properties of the thermodynamic structure of the atmospheres of different stars and understand their causes. Methods. We ran comprehensive 3D radiation hydrodynamics simulations of the near-surface layers of six simulated stars of spectral type F3V to M2V with the MURa