The stability of coronal and prominence magnetic fields.
Abstract
The magnetic fields in prominences and active regions (coronal arcades) may be susceptible to a variety of instabilities. Ideal MHD instabilities are the fastest growing and criteria for checking stability are complicated by the line tying effect of the dense photosphere. The significance of the localised instabilities is not yet fully understood. The nonlinear coupling of these modes may give rise to an explosive instability, with the modes coupling to longer wavelengths, (Mondt and Weiland, 1985). On the other hand, if the modes saturate early, then the main effect of the instability may be an enhancement of transport coefficients. Nonetheless, the author gives an equation which provides a simple test for the stability of cylindrical magnetic fields.
- Publication:
-
NASA Conference Publication
- Pub Date:
- December 1986
- Bibcode:
- 1986NASCP2442..457H
- Keywords:
-
- Magnetic Fields;
- Magnetohydrodynamic Stability;
- Mathematical Models;
- Prominences;
- Solar Corona;
- Ballooning Modes;
- Boundary Value Problems;
- Linear Equations;
- Photosphere;
- Solar Physics;
- Magnetic Fields:Solar Corona;
- Magnetic Fields:Solar Prominences;
- Magnetohydrodynamics:Solar Corona;
- Solar Corona:Magnetic Fields;
- Solar Corona:Magnetohydrodynamics;
- Solar Prominences:Magnetic Fields