Dynamic Formation of Stressed Coronal Magnetic Fields.
Final rept. 2 Nov 84-2 Feb 86,
CALIFORNIA UNIV IRVINE DEPT OF PHYSICS
Pagination or Media Count:
Magnetic fields in the quiescent solar corona usually remain connected to photospheric subcoronal fields. Since the ratio between the plasma and magnetic pressures satisifies beta somewhat 1 below the corona, the frozen in field in this high inertia region is easily moved about by the continual motion of the photospheric plasma. In the corona, however, beta somewhat 0.1 and magnetic effects dominate. The response of coronal fields to photospheric motion is simulated by subjecting a coronal magnetic cylinder, with an initially uniform axial field, to a radially varying twist at the end plastes. Azimuthal symmetry is assumed, and the time dependent MHD equations are solved numerically for a specified end plate rotation.