Magnetohydrodynamic thermal instabilities in cool inhomogeneous atmospheres

Details Magnetohydrodynamic thermal instabilities in cool inhomogeneous atmospheres Magnetohydrodynamic thermal instabilities in cool inhomogeneous atmospheres

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..798b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 798-805. Research supported by the Consiglio Nazion

Other

10

Current Density, Magnetohydrodynamic Stability, Stellar Atmospheres, Stellar Coronas, Stellar Magnetic Fields, Thermal Instability, Convection Currents, Coronal Loops, Main Sequence Stars, Ohmic Dissipation, Photosphere, Resistance Heating

Scientific paper

The stability of magnetic loops to current-driven filamentation instabilities is investigated. The unperturbed atmosphere is assumed to be composed of an (upper) isothermal optically thin low-density portion and a (lower) higher-density portion which is in radiative equilibrium; in both cases, the atmosphere is in hydrostatic equilibrium, so that gravitational stratification is taken into account. In order to provide specific equilibrium conditions for evaluation of the dispersion relation, conditions appropriate for the surface of a solar-type star are adopted; i.e., a fairly low temperature (T = 5000 K) appropriate for a 'precoronal' state associated, for example, with magnetic flux emerging from photospheric levels under the action of magnetic buoyancy. A linear stability analysis is performed, and numerical results show that physically plausible current densities, which would be generated by typical loop-footpoint motions, are effective in driving MHD instabilities in such a plasma. The instability growth rates are strongly dependent on the assumed current density distribution and on the density scale height.

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