Solving the system of Radiation Magnetohydrodynamics | for solar physical simulations in 3d. This item is unavailable.Solving the system of Radiation Magnetohydrodynamics | for solar physical simulations in 3d

We present a Finite-Volume scheme for solving the equations of radiation magnetohydrodynamics. This system is for example used to model the plasma in the solar convection zone and in the solar photosphere. The starting point is a basic scheme for conservation laws. We first study the convergence of the scheme applied to a model problem for the full system of radiation magnetohydrodynamics. We then present modifications of the base scheme which make it possible to approximate the system with an arbitrary equation of state, reduce errors due to a violation of the divergence constraint on the magnetic field, and lead to an improved accuracy in the approximation of solution near an equilibrium state. These modifications are essential for an accurate simulation of processes in the solar atmosphere. For simulations in the solar photosphere, we additionally have to take the radiation intensity into account. A scheme for solving the radiation transport equation is thus a further focus of this study.

From 1992 to 1998 Andreas Dedner studied Mathematics at theUniversity of Freiburg. In 1997 he started to develop schemes forsolar physical applications as part of the priority researchprogram ANumE funded by the DFG. The project ended 2003 with thisdissertation, which was awarded the Ferdinant von Lindemann Price.