Modelling the magnetic field of a flaring active region

Details Modelling the magnetic field of a flaring active region Modelling the magnetic field of a flaring active region

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..431a&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Physics

1

Solar Corona, Solar Flares, Magnetic Fields

Scientific paper

An M1.3 solar flare was observed on April 12th, 2000 in EUV by TRACE. Photospheric magnetograms were also obtained from observations by SOHO/MDI around the time of the flare. The magnetic field of the active region in which the flare occurred has been reconstructed from the MDI data, using a Green's function approach. A constant-α force-free approximation was used to model the region as a whole, α being chosen to give the best match to the observed coronal emission. The resulting structure included a dome of field connected to the flaring region. The existence of this dome had been suggested by an observed brightening of its coronal footpoints during the flare.

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