Numerical simulations of surface convection in a late M-dwarf
Based on detailed 2D and 3D numerical radiation-hydrodynamics (RHD)simulations of time-dependent compressible convection, we have studiedthe dynamics and thermal structure of the convective surface layers of aprototypical late-type M-dwarf (Teffapprox 2800 K, log g=5.0,solar chemical composition). The RHD models predict stellar granulationqualitatively similar to the familiar solar patt
