Evolving force-free magnetic fields. II - Stability of field configurations and the accompanying motion of the medium

Details Evolving force-free magnetic fields. II - Stability of field configurations and the accompanying motion of the medium Evolving force-free magnetic fields. II - Stability of field configurations and the accompanying motion of the medium

Nov 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..988l&link_type=abstract

Astrophysical Journal, Part 1, vol. 217, Nov. 1, 1977, p. 988-998.

Physics

36

Force-Free Magnetic Fields, Magnetic Field Configurations, Magnetohydrodynamic Stability, Photosphere, Solar Atmosphere, Solar Magnetic Field, Evolution (Development), Flow Distribution, Kinematic Equations, Mass Transfer, Plasma Dynamics, Solar Flares, Solar Physics

Scientific paper

Two features of magnetic field evolution in the solar atmosphere are examined for understanding solar flare phenomena. A stability analysis of the force-free configurations of the magnetic field in Paper I (1977), treated as static fields with their foot points rooted in the photosphere, reveals that they are stable when subject to infinitesimal perturbations which depend on two Cartesian coordinates. As a result, the quasi-static evolution of intense magnetic fields in the solar atmosphere may be understood in terms of successive infinitesimal displacements of photospheric magnetic foot points and the relaxation to a new stable force-free configuration following each infinitesimal displacement of magnetic foot points. Furthermore, a kinematic approach is described for obtaining information on the plasma motion during the evolution of a magnetic field. The kinematic velocities that satisfy the governing induction equation are found to have contrasting flow patterns associated with qualitatively different mass transport.

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