Magnetic field potential approximation and penumbral fine structure before the white-light flare of July 4, 1974

Details Magnetic field potential approximation and penumbral fine structure before the white-light flare of July 4, 1974 Magnetic field potential approximation and penumbral fine structure before the white-light flare of July 4, 1974

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983baicz..34..282k&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 34, no. 5, 1983, p. 282-285.

Astronomy and Astrophysics

Astronomy

Penumbras, Solar Flares, Solar Magnetic Field, Field Strength, Photosphere, Polarity

Scientific paper

A comparison is made of the horizontal solar magnetic field component distribution calculated at the photosphere, with the penumbral fine structure of the large active group in the McMath active region 13 043 before the white-light flare of July 4, 1974. The magnetic field is calculated as a potential approximation taking into account the shape of individual spots in the group. Good agreement was found for the peripheral portions of the flare activity regions, although strong deviations were found in and near the location of white-light flare. The discrepancies in the flare location support the conclusion that the magnetic field structure in these regions before the white-light flare have a non-potential component: that electric currents are present even at the photospheric level. The disappearance of the discrepancies implies that the direction of the penumbral fibrils after the flare corresponds more to that of the potential magnetic field approximation.

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