Magnetic field configuration of active region NOAA 6555 at the time of a long-duration flare on 23 March 1991 - An Exception to Standard Flare Reconnection Model

Details Magnetic field configuration of active region NOAA 6555 at the time of a long-duration flare on 23 March 1991 - An Exception to Standard Flare Reconnection Model Magnetic field configuration of active region NOAA 6555 at the time of a long-duration flare on 23 March 1991 - An Exception to Standard Flare Reconnection Model

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999soph..188..345c&link_type=abstract

Solar Physics, v. 188, Issue 2, p. 345-364 (1999).

Physics

6

Scientific paper

The high-resolution Hα images observed during the decay phase of a long-duration flare on 23 March 1991 are used to study the three-dimensional magnetic field configuration of the active region NOAA 6555. Whereas all the large flares in NOAA 6555 occurred at the location of high magnetic shear and flux emergence, this long-duration flare was observed in the region of low magnetic shear at the photosphere. The Hα loops activity started soon after the maximum phase of the flare. There were a few long loop at the initial phase of the activity. Some of these were sheared in the chromosphere at an angle of about 45° to the east-west axis. Gradually, an increasing number of shorter loops, oriented along the east-west axis, started appearing. The chromospheric Dopplergrams show blue shifts at the end points of the loops. By using different magnetic field models, we have extrapolated the photospheric magnetograms to chromospheric heights. The magnetic field lines computed by using the potential field model correspond to most of the observed Hα loops. The height of the Hα loops were derived by comparing them with the computed field lines. From the temporal evolution of the Hα loop activity, we derive the negative rate of appearance of Hα features as a function of height. It is found that the field lines oriented along one of the neutral lines were sheared and low lying. The higher field lines were mostly potential. The paper also outlines a possible scenario for describing the post-flare stage of the observed long-duration flare.

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