Statistics – Computation
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..111..309z&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 111, no. 2, 1987, p. 309-331. DFG-supported research.
Statistics
Computation
72
Magnetohydrodynamics, Solar Corona, Solar Flares, Solar Magnetic Field, Solar Wind, Boundary Conditions, Boundary Value Problems, Computational Astrophysics, Perturbation Theory, Pressure Gradients
Scientific paper
The author applies the model of quasistatic equilibrium sequences to describe the time development of magnetic field structures in the plasma of the solar corona, and to determine onset points of a dynamical evolution. The representation of the magnetic field by Euler potentials provides a realistic modeling of the photospheric boundary conditions. He presents a numerical method suited for the computation of magnetohydrodynamic equilibrium states and for analysing their stability against perturbations within ideal MHD. Pressure and magnetic footpoint displacement can be prescribed separately as boundary conditions. The author considers magnetic arcade structures typical for large two-ribbon flares. The results indicate that a finite pressure gradient seems to be essential for the existence of onset points. Furthermore, it is shown that magnetic shear destabilizes for intermediate values, but can have a stabilizing effect for a large amount of shear.
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