An energy method for the stability of solar magnetohydrostatic atmospheres

Details An energy method for the stability of solar magnetohydrostatic atmospheres An energy method for the stability of solar magnetohydrostatic atmospheres

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984gapfd..28..223h&link_type=abstract

Geophysical and Astrophysical Fluid Dynamics (ISSN 0309-1929), vol. 28, April 1984, p. 223-241.

Physics

Fluid Dynamics

18

Magnetic Field Configurations, Magnetohydrodynamic Stability, Magnetohydrostatics, Potential Energy, Solar Corona, Solar Magnetic Field, Coronal Loops, Plasma Equilibrium, Solar Flares

Scientific paper

The energy method of Bernstein et al. (1958) was used by Schindler et al. (1983) to derive a useful form of the linearised potential energy for coronal arcades. The basic state magnetic field and plasma are assumed to be in magnetohydrostatic equilibrium and independent of variations along the length of the arcade. A sufficient condition for stability is derived and is applied to two particular magnetic structures. When the axial field component vanishes, this condition becomes necessary and sufficient.

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