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Structure and Equilibrium of Coronal Magnetic Fields

Published online by Cambridge University Press:  19 July 2016

A. A. Van Ballegooijen
A. A. Van Ballegooijen*
Affiliation:
Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge, MA 02138, U.SA.

Abstract

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In “closed” magnetic structures (i.e., coronal loops) the random shuffling of magnetic footpoints in the photosphere causes twisting and braiding of field lines in the corona. If the motions are sufficiently slow, the coronal field evolves through a sequence of force-free equilibrium states. Numerical simulations are presented for a simplified model in which the overall curvature of the coronal loop is neglected. It is shown that magnetic fine structures develop on spatial scales significantly smaller than those of the imposed “photospheric” velocity field.

Type
VII. Magnetic Reconnection and Coronal Evolution
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 303 - 308
Copyright
Copyright © Kluwer 1990 

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