Statistics – Computation
Scientific paper
May 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..830m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 830-847.
Statistics
Computation
196
Coronal Loops, Magnetohydrodynamic Flow, Solar Corona, Solar Flares, Solar Magnetic Field, Computational Astrophysics, Dynamic Characteristics, Kinetic Energy
Scientific paper
Calculations of the long-term dynamical evolution of a solar coronal magnetic field arcade which is subjected to shearing photospheric flows are presented. The evolution is obtained by numerical solution of a subset of the resistive magnetohydrodynamic equations. For a simplified model of the bipolar magnetic field observed in the solar corona, it is found that photospheric flow produces a slow evolution of the magnetic field, with a buildup of magnetic energy. For certain photospheric shear profiles, the field configuration produced is linearly unstable to an ideal magnetohydrodynamic mode when the shear exceeds a critical value. The nonlinear evolution of this instability shows the spontaneous formation of current sheets. Reconnection of the magnetic field produces a rapid release of magnetic energy. The major fraction of the energy is dissipated resistively, while a small fraction is converted into kinetic energy of an ejected plasmoid. The relevance of these results to two-ribbon flares is discussed.
Barnes Daniel C.
Mikic Zoran
Schnack Dalton D.
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