2 Assumptions for the GRB mechanism

During accretion of interstellar plasma onto a SBH, magnetic fields strengthen up to 10¹¹ - 10¹² G and probably form a regular magnetosphere [6, (Bisnovatyj-Kogan & Ruzmaikin 1976;] [11, Kardashev 1995;] [9, Chakrabarti 1996;] [3, Beskin 1997).]

In the magnetosphere there are local inhomogeneities similar to those of Sun and flare stars [7, (Byrne 1992;] [18, Priest 1994)] but with magnetic fields up to 10¹⁴ G.

The energy of these inhomogeneities as the result of spontaneous development of plasma instabilities turns into energy of fast particles and into anomalous heating. The GRB is therefore the burst of photons that have been generated as the result of such a process. We think this is an analog of solar flares and flashes of UV Ceti type stars and of the activity in X-ray binaries with compact components (for some evidence of this see [12, Katsova & Livshits 1991;] [20, Rotschild et al. 1974;] [, Meekins 1984;] [2, Bartolini et al. 1994).]

The distribution of these flares (as well as GRBs) as a function of energy has a universal character, i.e. ${{\rm d}N(E) \over {\rm d}E} \propto E^{-\beta}$,where $\beta= 1.7 - 1.8$.Such a universality is caused by the percolation nature of the stability break in active regions [10, (Feder 1988;] [23, Wentzel & Seiden 1992;] [19, Pustil'nik 1997).] Electrons (or positrons) and protons are accelerated in processes of dissipation of magnetic energy inhomogeneities up to $\gamma \sim 10^3 - 10^6$. Particle streams are beamed as result of one- and two-dimensions structure of magnetic field reconnection regions. They can change the direction of the motion very rapidly. The radiation is generated by these particles in magnetic fields near SBHs and in the interstellar medium (ISM). The emission is beamed as result of the stream sharpness and of the relativistic motion.