A solar flare in the Fe I 5324 line on 24 June, 1993.

Details A solar flare in the Fe I 5324 line on 24 June, 1993. A solar flare in the Fe I 5324 line on 24 June, 1993.

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..168..135l&link_type=abstract

Solar Physics, Vol. 168, No. 1, p. 135 - 143

Physics

2

Solar Flares: Heating, Solar Flares: White-Light Flares, Solar Flares: Iron Lines

Scientific paper

A solar flare with both Hβ and Fe I 5324 emissions was observed in AR 7529 on 24 June, 1993 at the Beijing Astronomical Observatory. Calculations show that the Fe I 5324 emission region of the flare was located in the low photosphere at a height of about 180 km above τ5000 = 1, which is lower than many previous studies of white-light flares. The synthetic analyses from various features of the flare lead to the following possible exciting mechanism of the Fe I 5324 flare: owing to the flow of energetic electrons from the corona and probably also the thermal conduction downward into the lower atmosphere, a condensation with a temperature higher than that below it was formed near the transition region. Then the low photosphere was heated through backwarming. The Fe I 5324 flare occurred as an indicator of the excitation in the low photosphere.

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