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The thermal instability in a sheared magnetic field - Filament condensation with anisotropic heat conductionThe condensation-mode growth rate of the thermal instability in an empirically motivated sheared field is shown to depend upon the existence of perpendicular thermal conduction. This typically very small effect (perpendicular conductivity/parallel conductivity less than about 10 to the -10th for the solar corona) increases the spatial-derivative order of the compressible temperature-perturbation equation, and thereby eliminates the singularities which appear when perpendicular conductivity = 0. The resulting growth rate is less than 1.5 times the controlling constant-density radiation rate, and has a clear maximum at a cross-field length of order 100 times and a width of about 0.1 the magnetic shear scale for solar conditions. The profiles of the observable temperature and density perturbations are independent of the thermal conductivity, and thus agree with those found previously. An analytic solution to the short-wavelength incompressible case is also given.
Document ID
19840060493
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Van Hoven, G.
(California Univ. Irvine, CA, United States)
Mok, Y.
(California, University Irvine, CA, United States)
Date Acquired
August 12, 2013
Publication Date
July 1, 1984
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 282
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
84A43280
Distribution Limits
Public
Copyright
Other

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