Dynamics of solar coronal magnetic fields

Details Dynamics of solar coronal magnetic fields Dynamics of solar coronal magnetic fields

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...383..420d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 383, Dec. 10, 1991, p. 420-430. Research supported by NASA and U.S. Navy.

Physics

25

Magnetohydrodynamics, Solar Activity, Solar Corona, Solar Magnetic Field, Digital Simulation, Navier-Stokes Equation, Photosphere, Runge-Kutta Method, Solar Physics

Scientific paper

A 3D time-dependent numerical simulation of the foot-point stressing of coronal magnetic field was developed in order to relate coronal activity with the stressing of the coronal magnetic field by foot-point motions at the photosphere. The results of the simulation did not reveal magnetic reconnection, kinking, or the formation of concave-up magnetic field lines suitable for prominence formation. It is concluded that, contrary to many models, photospheric twisting of a single arcade does not lead to the type of processes required to explain solar activity.

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