I give here a short review of some of the main problems of the magnetic theories for the flare origin. I point out that the magnetic theories are unable to solve the problems of the energetics, height and compactness of the acceleration region, compresslve inflows, magnetic field structures, particle numbers, preflare upflows and the global cause of the flare origin. Then I outline the convective flare theory which have proposals for the solutions of these problems. I show here what is the role of the magnetic field at flare origins in the frame of the convective flare theory. The convective flare theory gives a deeper level understanding than the magnetic theories and therefore it also can supply us with the derivation of some input parameters and assumptions used for the magnetic theories and so it offers a wider perspective to understand the physics of the explosive astrophysical processes.

We have computed kineamtic dynamo models for the Sun making realistic assumptions about the different induction effects. Recent results of helioseismology are used to infer the differential rotation. By changing the value of the angular velocity at the bottom of the convection zone in the models we find more or less agreement with the observations.