  High-resolution observations show the fine structure of the global
equilibrium magnetic field configuration in solar atmosphere to be essentially
different from that assumed in the traditional 'potential + force-free' field
scenarios. The interacting large-scale structures of fine field elements are
separated by numerous non-force-free elements (tangential discontinuities)
which are neglected in the traditional field picture. An incorporation of these
elements into the model implies a dynamical rather than statical character of
equilibrium of the field configuration. A transition of the system into flaring
can be triggered by the ballooning mode of flute instability of prominences
or/and coronal condensations. Tearing-mode and MHD instabilities as well as the
effects of overheating of the turbulent current sheet prevent the field from
stationary reconnection as it is adopted in the traditional scenario. We
speculate around the assumption that the energy release in active regions is
governed by the same scenario as dynamical current percolation through a random
network of resistors in which the saltatory resistance is controlled by local
current.
