Dynamics of Solar Coronal Magnetic Fields
Abstract
A 3D time-dependent numerical simulation of the foot-point stressing of coronal magnetic field was developed in order to relate coronal activity with the stressing of the coronal magnetic field by foot-point motions at the photosphere. The results of the simulation did not reveal magnetic reconnection, kinking, or the formation of concave-up magnetic field lines suitable for prominence formation. It is concluded that, contrary to many models, photospheric twisting of a single arcade does not lead to the type of processes required to explain solar activity.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- December 1991
- DOI:
- 10.1086/170799
- Bibcode:
- 1991ApJ...383..420D
- Keywords:
-
- Magnetohydrodynamics;
- Solar Activity;
- Solar Corona;
- Solar Magnetic Field;
- Digital Simulation;
- Navier-Stokes Equation;
- Photosphere;
- Runge-Kutta Method;
- Solar Physics;
- Solar Physics;
- HYDROMAGNETICS;
- SUN: CORONA;
- SUN: MAGNETIC FIELDS