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Current-driven magnetohydrodynamic thermal instabilities in sheared fieldsApproximate analytic solutions are sought for the dispersion relation for the MHD stability of magnetized medium in current-driven filamentation modes such as those observed in the solar atmosphere. The magnetic field is assumed to have a self-consistent sheared equilibrium structure. The analysis is carried out in the small wavenumber regime, where shear length is similar to the mode wavelength. Instability is found to depend on the ratio between the thermal and magnetic diffusivities, i.e., the Prandtl number, which identifies the unstable transverse wavenumbers. The instability conditions are expressed in an algebraic equation amenable to numerical solution. Results are provided from use of the model to determine the maximum growth rate and typical scale lengths of instabilities in a precoronal atmosphere and the lower transition region.
Document ID
19870044567
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Bodo, G.
(Torino Osservatorio Astronomico, Turin, Italy)
Ferrari, A.
(Osservatorio Astronomico Turin, Italy)
Massaglia, S.
(Torino, Universita Turin, Italy)
Rosner, R.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 13, 2013
Publication Date
February 1, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 313
ISSN: 0004-637X
Subject Category
Plasma Physics
Accession Number
87A31841
Distribution Limits
Public
Copyright
Other

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