THE SOLAR-FLARE OF 1992 AUGUST 17 23 58-UT

A small flare (C4.3 in the GOES X-ray class) was well observed by all of the instruments on board Yohkoh. The X-ray light curves have double peaks which are about 5 min apart. Until the first peak from flare on set, four compact areas brighten up in the soft X-ray region, which ar e aligned almost on one straight line. We regard them as being footpoi nts of two sets of loops, which are identifiable in soft X-ray images, since their locations match those of hard X-ray sources. Indeed, afte r the second peak, the temporal behavior of the temperature and emissi on measure at each point is consistent with the existence of two such loops. Comparing our results with recent MHD simulations; we propose a possible scenario for this flare that is based on the coalescence of two loops.