Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...382..677s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 382, Dec. 1, 1991, p. 677-687.
Astronomy and Astrophysics
Astrophysics
44
Force-Free Magnetic Fields, Hydrodynamic Equations, Shear, Solar Corona, Solar Magnetic Field, Magnetic Field Configurations, Magnetohydrodynamics, Photosphere, Solar Atmosphere, Stellar Evolution
Scientific paper
Numerical solutions of the compressible MHD equations are used here to simulate the evolution of an initially force-free magnetic field in a static corona as a result of slow photospheric motion of the magnetic field footpoints. Simulations have been completed for values of plasma beta from 0.1 to 0.5, maximum shear velocities from 0.5 to 10.3 km/s, and with various amounts of resistive and viscous dissipation. In all cases the evolution proceeds in two qualitatively different stages. In the earlier stage, the field evolves gradually with the field lines, expanding outward at a velocity not unlike the shear velocity. Then, the field begins to expand much more rapidly until it reaches velocities exceeding a characteristic Alfven velocity. Inclusion of the thermodynamics, gravity, and compressibility is shown to have only a quantitative effect on the onset of the eruptive phase, illustrating that the primary interactions are between the dynamics and the magnetic field evolution.
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