Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..432b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 1, 1987, p. 432-439. Research supported by the Ministero della Pu
Astronomy and Astrophysics
Astrophysics
7
Magnetohydrodynamic Stability, Plasma Currents, Shear Flow, Solar Corona, Thermal Instability, Conductive Heat Transfer, Plasma Conductivity, Reynolds Number
Scientific paper
Approximate 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.
Bodo Gianluigi
Ferrari Aldo
Massaglia Silvano
Rosner Robert
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