Abstract
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 language | English |
|---|---|
| Pages (from-to) | 223-241 |
| Journal | Geophysical and Astrophysical Fluid Dynamics |
| Volume | 28 |
| DOIs | |
| Publication status | Published - 1 Apr 1984 |
Keywords
- Magnetic Field Configurations
- Magnetohydrodynamic Stability
- Magnetohydrostatics
- Potential Energy
- Solar Corona
- Solar Magnetic Field
- Coronal Loops
- Plasma Equilibrium
- Solar Flares