Changes of Magnetic Structure in 3-D Associated with the X3.4 Flare of 2006 December 13

Details Changes of Magnetic Structure in 3-D Associated with the X3.4 Flare of 2006 December 13 Changes of Magnetic Structure in 3-D Associated with the X3.4 Flare of 2006 December 13

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp51c..02j&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP51C-02

Physics

7509 Corona, 7519 Flares, 7524 Magnetic Fields

Scientific paper

Recent observations demonstrated that sunspot structure can change rapidly and irreversibly after flares. One of the most puzzling results is the increase in magnetic shear around flaring magnetic polarity inversion line after flares. However, all these observations were made at the photosphere level. We study the altitude variation of the non-potentiality of the magnetic fields associated with the 4B/X3.4 flare of 2006 December 13. The vector magnetograms with unprecedented quality from Hinode before and after the flare are used as the boundary conditions to extrapolate the 3-dimensional non-linear force-free magnetic fields and the potential fields. The former are computed with the optimization algorithm and the latter with Green's function method. At the photosphere boundary, magnetic shear increases after the flare in a local area close to the flaring magnetic polarity inversion line. Two measures of the magnetic non-potentiality, the weighted mean shear θw and the total magnetic shear θwB, are calculated in this area at progressively higher altitude. By comparing their altitude variation profiles before and after the flare, we find that the non-potentiality of the local area increases after the flare below ~8 Mm and decreases from that height to ~70 Mm. Beyond 70 Mm, the magnetic fields approach potential for both times.

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