Abstract
The application of stability theory to quiescent solar prominences is examined, reviewing the results of recent investigations. The governing equations for the primary MHD instabilities (kink-mode, sausage-mode, and Rayleigh-Taylor) are presented; normal-mode, energy-method, and nonequilibrium approaches to their solution are outlined; and particular attention is given to the effect of the dense photosphere, ballooning modes, coronal arcades, distributed current models and eruptive instability, localized modes and small-scale structure, and arcades containing a current sheet. Also discussed are the problem of thermal stability, resistive instabilities and tearing modes, the effect of line tying, and a simple model describing prominence eruption and coronal mass ejection.
| Original language | English |
|---|---|
| Pages (from-to) | 167-191 |
| Journal | IN: Dynamics and structure of quiescent solar prominences; Proceedings of the Workshop, Palma de Mallorca, Spain, Nov. 1987 (A89-51201 22-92). Dordrecht, Kluwer Academic Publishers, 1989 |
| Volume | 150 |
| DOIs | |
| Publication status | Published - 1987 |
Keywords
- Magnetic Field Configurations
- Magnetohydrodynamic Stability
- Solar Prominences
- Coronal Loops
- Plasma Cylinders
- Solar Corona
- Solar Magnetic Field
- Tearing Modes (Plasmas)