Abstract
Hydrodynamic instabilities are the source of many interesting physical phenomena in fluid dynamics. In this paper we considermagnetohydrodynamic (MHD)instabilities, in particular of Rayleigh-Taylor type. Our numerical studies are motivated by a specific application in solar physics: The development of sun spots — which can be observed from earth — is connected to magnetic field concentrations which develop in the solar convection zone. Driven by magnetic forces, these so-called flux tubes rise through the atmosphere. They are fragmented due to Rayleigh-Taylor type instabilities, and their initially simple structure is perturbed by secondary instabilities of Kelvin-Helmholtz type. An efficient numerical simulation of this complex scenario (large area with small scale structures) requires the incorporation of techniques like local adaptivity and parallelization. At the same time the code must be able to resolve the two basic instabilities in a reliable manner. We focus on these two issues and their interplay.
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Dedner, A., Kröner, D., Rohde, C., Wesenberg, M. (2001). MHD Instabilities Arising in Solar Physics: A Numerical Approach. In: Freistühler, H., Warnecke, G. (eds) Hyperbolic Problems: Theory, Numerics, Applications. International Series of Numerical Mathematics, vol 140. Birkhäuser, Basel. https://doi.org/10.1007/978-3-0348-8370-2_29
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DOI: https://doi.org/10.1007/978-3-0348-8370-2_29
Publisher Name: Birkhäuser, Basel
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