Thermal instability in slab geometry in the presence of anisotropical thermal conduction

Details Thermal instability in slab geometry in the presence of anisotropical thermal conduction Thermal instability in slab geometry in the presence of anisotropical thermal conduction

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..131...79v&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 131, Jan. 1991, p. 79-105.

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Computation

14

Magnetohydrodynamic Stability, Solar Flares, Solar Prominences, Thermal Instability, Thermal Plasmas, Boundary Conditions, Computational Astrophysics, Magnetic Fields, Plasma Layers, Thermal Conductivity

Scientific paper

The thermal stability of a magnetized plasma is investigated under solar coronal conditions. The equilibrium structure of the plasma is approximated by a one-dimensional slab configuration. Taking into account optically thin plasma radiation and anisotropic thermal conduction, the configuration is investigated in thermal instability. The thermal conduction perpendicular to the magnetic field is taken to be small but nonzero, and the plasma column is placed in a low-density background stretching towards infinity. The major effect of this change from the classic rigid wall boundary conditions usually applied is on the eigenfunctions rather than on the growth rate. Essentially, the perpendicular field structure introduces a field-aligned fine structure. It is also shown that thermal instability in a slab model in the presence of perpendicular thermal conduction is only possible if the inner plasma has the shortest thermal instability time scale.

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