corresponding objects (observed both in the ultra–violet and in the soft X–rays), which are situated very close to us. These may be only the objects which are in the bounds of the Local Bubble. Hence our model estimates refer also only to the nearest space, where, in particular, the distances to the supposed sources are determined only by their average spatial density ($\approx 0.001-0.036/{\rm pc^{3}}$), if it is assumed to be approximately constant in a sphere of radius 100 pc. Thus, first of all from the observational point of view, we are interested in the local situation with the sources of [$\gamma$]{}–ray bursts of the bright (short and powerful) events for which the law of -3/2 in the distribution LogN/LogS is still valid (Kouveliotou et al., 1993; Fishman et al., 1994). Here we try to use a minimum of model assumptions referring to “Big Galactic models” (Hartmann, 1994) and, so, we are dealing here only with the nearest objects — potential sources of [$\gamma$]{}–ray bursts.

GRB790613 is just one of the most powerful short ($\approx 0.1$ s) events which was simultaneously observed with the help of V-12 SIGNE, V-11 KONUS and PVO at photon energies exceeding 100 keV ($\approx 0.1{\rm 