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EP: Fachverband Extraterrestrische Physik
EP 2: Sun and Heliosphere I
EP 2.2: Vortrag
Dienstag, 31. März 2020, 11:30–11:45, H-HS VIII
Magnetohydrostatic modelling of the solar atmosphere: Analytical solutions — •Thomas Wiegelmann1, Thomas Neukirch2, and Xiaoshuai Zhu1 — 1Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany — 2School of Mathematics and Statistics, University of St Andrews, St Andrews, KY169SS, United Kingdom
Our aim is to model the magnetic field and plasma environment in the solar atmosphere and use measured photospheric magnetograms as boundary condition. While the solar corona above active regions can be modelled under the assumption of a vanishing Lorentz-force, we have to consider plasma forces like the plasma pressure gradient force and gravity in the upper photosphere and chromosphere. Fully numerical solutions have been developed, but they are numerically expensive and require high resolution photospheric vector magnetograms as boundary conditions. Nevertheless analytical solutions in 3D are very useful for various reasons: 1.) They require only line-of-sight magnetograms as input. This is an advantage in the quiet Sun, where horizontal fields cannot be measured accurately. 2.) Computations are much quicker than for fully numerical approaches. 3.) New analytic solutions allow an accurate modelling of the transition between the magnetostatic chromosphere and the force-free corona. 4.) Analytic solutions are useful as initial state for numerical computations.