Solving the system of radiation magnetohydrodynamics for solar physical simulations in 3d [Elektronische Ressource] / Andreas Dedner

Albert-Ludwigs-Universit¨at Freiburg i. Br.Fakult¨at fur¨ Mathematik und PhysikSolving the System of RadiationMagnetohydrodynamicsfor solar physical simulations in 3dAndreas DednerDissertation zur Erlangung des Doktorgrades der Fakult¨at fur¨ Mathematik undPhysik der Albert-Ludwigs-Universitat¨ Freiburg im BreisgauBetreuer: Prof. Dr. Dietmar Kroner¨Abteilung fur¨ Angewandte MathematikFreiburg im Breisgau, April 2003Dekan : Prof. Dr. Rolf SchneiderReferenten : Prof. Dr. Dietmar Kr¨oner: Prof. Dr. Gerald Warnecke, Universit¨at MagdeburgDatum der Promotion : 22. September 2003Picture on title page:simulation of a circular slip stream. In the purely hydrodynamic setting the interface is unstable withrespect to perturbations (Kelvin–Helmholtz instability). By means of a sufficiently strong magneticfield that is tangential to the interface, this instability can be suppressed. For the simulation shownhere, the magnetic field is not yet strong enough so that the development of the Kelvin–Helmholtzinstabilities can be clearly seen. The large picture shows the density of the fluid. The two smallerpictures show the locally adapted grid (top) and the third component of the magnetic field (bottom)in a small section of the domain in the vicinity of the interface.AbstractIn this study we present a finite–volume scheme for solving the equa-tions of radiation magnetohydrodynamics in two and three space di-mensions.