A numerical study of flaring loop dynamics during magnetic reconnection Original Research Article

2.5-dimensional magnetic reconnection is numerically simulated for two cases, one with a high altitude of the reconnection point, the other with a low altitude. In the former case, bright loops appear to rise for a long time, with footpoints separating and the field lines below the bright loops shrinking. In the latter case, the bright loops cease to rise after a short period of reconnection and become rather stable. The results imply that the two types of solar flares, i.e., two-ribbon flares and compact flares, might be unified under a single magnetic reconnection model, where the height of the reconnection point leads to the bifurcation.