in the vicinity of the Sun (Paczynski, 1990). But, apparently, old neutron stars (ONS) only can not be potential sources of [$\gamma$]{}–ray bursts, basically because of their small number in the Galaxy, which demands repeated [$\gamma$]{}–ray bursts at the average rate of events registered per day in the BATSE experiment (Fishman et al., 1994; Hartmann, 1994). Proceeding from the population $N_{tot}\sim 10^{9}$ of galactic neutron stars born in the Galaxy disk with the velocity distribution observed for radio pulsars (as a result, part of them will leave for the halo), then the spatial density of our hypothetical objects must not be lower than $n_{ONS}\sim 0.001(N_{tot}/10^{9})\,\rm   pc^{-3}$, based on the estimates in (Paczynski, 1990) for a probable average density of old neutron stars in the Galaxy plane near the Sun.

We will use $\rm R = 10\rm~  km\ {\rm and }\ M = 1.4~  M_{\sun}$ for the radius and the mass of such an object — a hypothetical potential compact source of [$\gamma$]{}–ray burst, since we assume a kind of stable object or stable configuration, close to a “standard neutron” star at least by their gravitational properties. Below all estimates concern these parameters namely, though, naturally, the radii and masses of 