An energy method for the stability of solar magnetohydrostatic atmospheres

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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.
Original languageEnglish
Pages (from-to)223-241
JournalGeophysical and Astrophysical Fluid Dynamics
Publication statusPublished - 1 Apr 1984


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


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