The Atmospheric Dynamics in 2D and 3D Simulations of Stellar Surface Convection

Abstract

A pressing problem in our understanding of the structure and evolution of late-type stars is the lack of a reliable theory of convection. Convective flows transport mass, momentum, and energy, thus influencing the internal distribution of energy, chemical species, and angular momentum. They drive the stellar magnetic and oscillatory activity. Although the underlying physical principles are well known, the nonlinear and nonlocal character of the equations describing a radiating, partially ionized fluid has prevented the development of a closed analytical theory.