Solar flares driven by magnetic reconnection

BAGALÁ. L.G.; MANDRINI, C.H.; ROVIRA, M.G.; DÉMOULIN, P.

Tandil

Workshop; VIII Latin-American Workshop on Plasma Physics; 1998

Universidad Nacional del Centro

In this work we present a study of the flaring active region (AR) 7031. We study the morphology of the Halpha emission for the two largest flares and we compare this morphology with the evolution and topology of the magnetic field. Using the Quasi-Separatrix Layers Method (QSLM), we explain why the flares brightened in different parts of the AR. Our model let us conclude that these two flares occur due to the interaction of different structures of the same magnetic bipole. Although this interaction could be traced in the computed topology before the flares, the energy release switched on or off in one site or the other of the AR.