Quasi-static evolution of coronal magnetic fields

Details Quasi-static evolution of coronal magnetic fields Quasi-static evolution of coronal magnetic fields

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...384..305l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 384, Jan. 1, 1992, p. 305-318.

Physics

21

Coronal Loops, Solar Magnetic Field, Stellar Physics, Magnetohydrodynamic Stability, Solar Corona

Scientific paper

A formalism is developed to describe the purely quasi-static part of the evolution of a coronal loop driven by its footpoints. This is accomplished under assumptions of a long, thin loop. The quasi-static equations reveal the possibility for sudden 'loss of equilibrium' at which time the system evolves dynamically rather than quasi-statically. Such quasi-static crises produce high-frequency Alfven waves and, in conjunction with Alfven wave dissipation models, form a viable coronal heating mechanism. Furthermore, an approximate solution to the quasi-static equations by perturbation method verifies the development of small-scale spatial current structure.

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