Using eighteen years of observations at Big Bear, we summarize the development of δ spots and the great flares they produce. We find δ groups to develop in three ways: eruption of a single complex active region formed below the surface, eruption of large satellite spots near (particularly in front of) a large older spot, or collision of spots of opposite polarity from different dipoles. Our sample of twenty-one δ spots shows that once they lock together, they never separate, although rarely an umbra is ejected. The δ spots are already disposed to their final form when they emerge. The driving force for the shear is spot motion, either flux emergence or the forward motion of p spots in an inverted magnetic configuration.
δ spots, preferentially Types 1 and 2.
Umbrae obscured by Hα emission.
Bright Hα emission marking flux emergence and reconnection.
Greatly sheared magnetic configurations, marked by penumbral and Hα fibrils parallel to the inversion line.
We assert that with adequate spatial resolution one may predict the occurrence of great flares with these indicators.
KeywordsFlare Fibril Active Region Opposite Polarity Forward Motion
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