The magnetic field twist and the flare occurrence rate in a solar active region

Details The magnetic field twist and the flare occurrence rate in a solar active region The magnetic field twist and the flare occurrence rate in a solar active region

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989chjss...9..206l&link_type=abstract

Chinese Journal of Space Science (ISSN 0254-6124), vol. 9, July 1989, p. 206-215. In Chinese, with abstract in English.

Mathematics

1

Magnetic Field Configurations, Solar Activity, Solar Flares, Solar Magnetic Field, Force-Free Magnetic Fields, Photosphere, Stellar Models, Sunspots

Scientific paper

The solar active region McMath 12094 of October 1972 is taken as an example in this study. Adopting a model of constant alpha force-free magnetic field for the region and taking the observed photospheric longitudinal magnetic field as the boundary condition, the values of force-free factor alpha, which represent the average level of magnetic twist in the region, are calculated for the four days when the region was near the center of solar disk (October 28-31). Using these alpha values, the three-dimensional configurations of the lines of magnetic force are extrapolated. Based on these data, the evolutionary characteristics of the magnetic field as well as the relation between the magnetic field twist and the flare occurrence rate are discussed. Finally, the electric current in the preceeding sunspot A of the region, the electric current density, and the stored magnetic energy caused by the counterclockwise rotation of sunspot A are estimated under the approximative model of a unipolar magnetic field.

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