Morphological characters of the two-ribbon flare of 1981 May 13 and their explanation

Details Morphological characters of the two-ribbon flare of 1981 May 13 and their explanation Morphological characters of the two-ribbon flare of 1981 May 13 and their explanation

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985cha%26a...9..119z&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 9, Issue 2, p. 119-123.

Astronomy and Astrophysics

Astrophysics

Scientific paper

We give a summary of the morphology of the two-ribbon flare of 1981 May 13. One striking feature is that the Ha flare began at about 0338' UT and the double-ribbon structure was formed about 0346, before the impulsive phase of the radio 3 cm burst at 04 11 UT. The 3 cm radio burst flux beginning at 03 33 UT showed only slow, stepwise increases lasting half an hour until the impulsive phase and this type of increase is usually regarded to be a typical thermal process. Each step in the radio flux corresponded to a variation in the Ha flare, showing that the radio and Hα emissions during this period came from the same thermal source. In this paper, we explain this behaviour in terms of Hyder's model: we think that the magnetic trough supporting the solar prominence rose for some reason, causing the prominence matter (the dark filaments) to fall along the magnetic lines and to hit the chromosphere and trigger off the flare. We give rough estimates of the energy density, the height of prominence and the infall matter at the different radio increments. We also give a qualitative explanation for the appearances of the single-peak structure in the radio burst at 0411 and the covering of the sunspot shortly after at 04 13 and propose several possible mechanisms.

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