Magnetohydrodynamic modeling of the solar corona

Details Magnetohydrodynamic modeling of the solar corona Magnetohydrodynamic modeling of the solar corona

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phflb...2.1450m&link_type=abstract

(APS Division of Plasma Physics, Annual Meeting, 31st, Anaheim, CA, Nov. 13-17, 1989) Physics of Fluids B (ISSN 0899-8221), vol.

Physics

Plasma Physics

24

Coronal Loops, Magnetohydrodynamics, Solar Corona, Stellar Models, Current Density, Photosphere, Solar Activity

Scientific paper

The ideal and resistive magnetohydrodynamic (MHD) model is used to examine the dynamics and structure of the solar corona. When the coronal magnetic field is deformed by photospheric flow it can evolve to states that become unstable to ideal MHD modes. The nonlinear evolution of these instabilities can lead to the generation of current sheets, field line reconnection, and energy release. The disruption of an arcade field and the kinking of coronal loops is described. The braiding of the large-scale coronal field by convective photospheric motions develops fine-scale structure in the magnetic field and leads to the development of intense current filaments. The resistive dissipation of these currents can provide an efficient coronal heating mechanism.

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