Periodical patterns in major flare occurrence and their relation to magnetically complex active regions

Details Periodical patterns in major flare occurrence and their relation to magnetically complex active regions Periodical patterns in major flare occurrence and their relation to magnetically complex active regions

Jan 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006adspr..38..886t&link_type=abstract

Advances in Space Research, Volume 38, Issue 5, p. 886-890.

Computer Science

Scientific paper

A periodical occurrence rate of major solar flares (observed in hard X-rays) of ˜24 days (synodic) was first reported by Bai (1987) [Bai, T. Distribution of flares on the sun superactive regions and active zones of 1980 1985. ApJ 314, 795 807, 1987] for the years 1980 1985. Here, we report a significant relation between the appearance of the 24-day period in major Hα flares and magnetically complex sunspot groups (i.e., including a γ and/or δ configuration). From synoptic maps of magnetograms (NSO/KP) patterns in the magnetic flux evolution are traced which might be the cause of the 24-day period observed in flare activity.

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