A TOPOLOGICAL APPROACH TO UNDERSTAND A MULTIPLE-LOOP SOLAR-FLARE

We analyze the UV and X-ray data obtained by the SMM satellite for the flare starting at 02:36 UT on November 12, 1980 in AR 2779. From a de tailed revision of the O V emission, we find that the observations are compatible with energy being released in a zone above the magnetic in version line of the AR intermediate bipole. This energy is then transp orted mainly by conduction towards the two distant kernels located in the AR main bipole. One of these kernels is first identified in this p aper. Accelerated particles contribute to the energy transport only du ring the impulsive phase. We model the observed longitudinal magnetic field by means of a discrete number of subphotospheric magnetic poles, and derive the magnetic field overall topology As in previous studies of chromospheric flares, the O V kernels are located along the inters ection of the computed separatrices with the photosphere. Especially w here the field-line linkage changes 'discontinuously', these kernels c an be linked in pairs by lines that extend along separatrices. Our res ults agree with the hypothesis of magnetic energy released by magnetic reconnection occurring on separatrices.