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MHD Analysis of the Evolution of Solar Magnetic Fields and Currents in an Active Region

Published online by Cambridge University Press:  04 August 2017

S. T. Wu ,
J. F. Wang  and
E. Tandberg-Hanssen
S. T. Wu
Affiliation:
The University of Alabama in Huntsville Huntsville, AL 35899, U. S. A.
J. F. Wang*
Affiliation:
The University of Alabama in Huntsville Huntsville, AL 35899, U. S. A.
E. Tandberg-Hanssen
Affiliation:
NASA/Marshall Space Flight Center Marshall Space Flight Center, AL 35812, U. S. A.
*
* Permanent Address: Dept. of Space Phys., Wu-Han University, China.

Abstract

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We have used a self-consistent magnetohydrodynamics model to study the evolution of solar magnetic fields in an active region. The problem has been cast as an initial boundary-value problem based on explicit mathematical formalism (i.e., method of projected characteristics), whereby a variety of horizontal photospheric motions can be treated. In this paper we deal specifically with photospheric shear motions in the active region. Our results show the evolution of the magnetic energy, the electric current systems, including the distributions of J⊥ (current perpendicular to the magnetic field) J| (current parallel to the magnetic field), the magnetic field configuration and a comparison between the build-up of magnetic energy in a pre-twisted field and in an initial untwisted field due to photospheric shearing motions. From these results we conclude that the energy build-up is confined within a certain region near the neutral line at the photospheric level. The possible location of the particle acceleration also can be studied.

Type
Session VII
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 487 - 490
Copyright
Copyright © Reidel 1985 

References

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