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Helical magnetohydrodynamic turbulence and the coronal heating problemNumerical simulations are used to investigate the relaxation of an unconfined, helically turbulent, fully three-dimensional magnetofluid, with conditions similar to those which are thought to result in the heating of the solar corona. In these simulations, the system evolves through a succession of force free states. After a relatively quiescent period of Ohmic decay, a phase of accelerated magnetic energy dissipation occurs. Some magnetic energy is transformed into kinetic energy, and the magnitude of entrophy created is a nontrival fraction of the mean square electric current. Concentrated vorticity structures are seen to play almost as important a role as electric current sheets in the heating process. Coincident with this accelerated dissipation process, a reorganization of the magnetic fields occurs, with transfer of magnetic energy to both shorter and longer wavelength modes than are initially present. The ratio of the magnetic field to the electric current density, alpha does not in general tend to assume a constant value in the force free regions during the evolution of the magnetofluid.
Document ID
19880059252
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Dahlburg, R. B.
(U.S. Navy, Naval Research Laboratory, Washington DC, United States)
Dahlburg, J. P.
(Dartmouth College Hanover, NH, United States)
Mariska, J. T.
(U.S. Navy, E. O. Hulburt Center for Space Research, Washington DC, United States)
Date Acquired
August 13, 2013
Publication Date
June 1, 1988
Publication Information
Publication: Astronomy and Astrophysics
Volume: 198
Issue: 1-2
ISSN: 0004-6361
Subject Category
Solar Physics
Accession Number
88A46479
Funding Number(s)
CONTRACT_GRANT: NAGW-710
Distribution Limits
Public
Copyright
Other

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