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Modeling Non-Potential Magnetic Fields in Solar Active Regions  

Monica Godha Bobra   Submitted: 2007-03-12 17:10

Many models aim to reproduce the non-linear force free fields in the solar corona; in this particular study, the magnetofrictional relaxation method is tested. This method produces non-linear force free fields based on line-of-sight magnetograms and ground-based Hα images to define the location of a filament, which is represented by a flux rope. The models are tested by comparing the results to TRACE observations of highly sheared, non-potential loop structures in four non-flaring active regions. We find that flux ropes with axial fluxes in the range of 0.2 to 4x1021 Maxwells are needed to reproduce the observed loops. For each event, we also derive estimates of the current, torsion parameter α and quasi-separatrix layer distributions, as well as the relative magnetic helicity and magnetic free energy.

Authors: M. G. Bobra, A. A. van Ballegooijen, E. E. DeLuca
Projects: SoHO-MDI,TRACE,Yohkoh-SXT

Publication Status: ApJ (submitted)
Last Modified: 2007-03-14 10:03
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Modeling Non-Potential Magnetic Fields in Solar Active Regions

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