Mathematics
Scientific paper
Dec 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..475s&link_type=abstract
In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 475-479 (SEE N87-20871 13-92)
Mathematics
Coronal Loops, Electric Fields, Magnetic Field Configurations, Mathematical Models, Photosphere, Solar Corona, Boundary Value Problems, Convection, Flow Distribution, Lorentz Force
Scientific paper
The response of coronal magnetic fields to photospheric motion is investigated using a time-dependent, two-dimensional MHD simulation. Starting with an initially uniform field, a circular section of the loop base is slowly rotated to represent the photospheric motion. The field lines at the base move with this flow in a manner consistent with the generated electric fields. The subsequent evolution of the field and flow can be characterized as passing through several distinct configurations. In the earliest phase the kinetic energy is negligible, and the current and field are parallel throughout most of the cylinder. This is followed by a period in which the field rotation increases, the axial field at and near the axis increases, and the axial field decreases in two cylindrical regions away from the axis. When the field in an appreciable portion of the cylinder has undergone one complete rotation, a rapid change in field configuration occurs with a large portion of the field making several rotations at large radii and a corresponding large reduction in the axial field.
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