ИСТИНА

Topology and dynamics of magnetic fluxes in ARs determine their flaring and SME activity. Magnetic field complexity and magnetic stresses in the solar atmosphere are likely controlled by motions of magnetic flux footpoints below the surface. Time sequences of points on the binary diagrams show intermittent behavior of ARs evolution: an AR passes with time from one quasi stationary state into other. These transformations are caused by emerging of new fluxes with appropriate realignment of AR magnetic field topology. Some of such transformations show good correlation with flares Corresponding time variation of parameters also show connection with flares. Post-flare magnetic flux depressions become restored very fast and their values (in energy) have order of magnitude of flare energy.