Speaker
Description
Realistic simulations of the solar upper convection zone and its atmospheric layers have become essential tools for unraveling complex magnetohydrodynamic processes in the Sun and complementing observational studies. These simulations also serve as laboratories for testing new ideas. One such idea involves incorporating partial ionization and other non-ideal effects - such as ambipolar diffusion, the Hall effect, and the Biermann battery effect - as potential mechanisms for explaining non-radiative heating in the solar chromosphere and transition region. In this lecture I will review numerical techniques and physical modules needed for producing a realistic simulation of the box-in-a-star style. I will discuss the role of the realistic equation of state, approximations for treatment of interaction of plasma and radiation, and heat conduction. I will review the major numerical codes routinely used for producing realistic solar simulations and will draw possible future lines for their development.
