Dynamics of solar coronal magnetic fields

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.