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Model prediction for an observed filament
Solar filaments/prominences are coronal structures in which the magnetic
field is extremely sheared. The field then contains a lot of free energy,
which can eventually be released through the opening of the field, thus
triggering a CME. From this point of view, the knowledge of the 3D configuration
of the field in these objects is crucial. It appears nowdays that the method
which is best adapted to this problem is the use of models which can directly
be compared with observations.
Authors: G. Aulanier, N. Srivastava, S.F. Martin
Organization: Naval Research Laboratory
Telephone: 202 404 1449
Address: Code 7675 A
Washington DC 20375
Above is background material for archival reference only.