MHD stability of incompressible coronal loops with radiative energy loss

Details MHD stability of incompressible coronal loops with radiative energy loss MHD stability of incompressible coronal loops with radiative energy loss

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...264..302a&link_type=abstract

Astrophysical Journal, Part 1, vol. 264, Jan. 1, 1983, p. 302-308.

Astronomy and Astrophysics

Astrophysics

6

Coronal Loops, Energy Dissipation, Magnetohydrodynamic Stability, Radiative Transfer, Solar Corona, Cylindrical Plasmas, Plasma Equilibrium

Scientific paper

Previous studies of the magnetohydrodynamic (MHD) stability of solar coronal loops have not taken into account the effects of radiative energy loss in the energy equation. However, since coronal loops continuously lose energy by radiation and heat conduction, it is important to understand how these energy loss mechanisms affect MHD stability. We investigate the problem assuming that a magnetic loop has cylindrical geometry. As a first step, stability is studied for a localized mode, and the result is applied to a specific equilibrium. We find that the radiative energy loss effect not only changes the growth rate of ideally unstable modes, but also alters the stability boundary predicted by ideal MHD theory.

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