burst GRB790613 we will show which distance limitation can be obtained from direct optical observations. In so doing we will use basically only the assumption of compact character of the supposed potential source of a [$\gamma$]{}–ray burst and the fact that the number of such objects in the vicinity of the Sun can not be greater than it is allowed by the estimates of hidden mass density. Further we use also the results of surveys and point–like observations in the soft X–rays by the ROSAT satellite.

Apparently, similar objects, single pulsars Geminga and PSR0656+14 with relatively low surface temperatures and probably situated in the vicinity of the Sun have already been observed in the optical (Halpern & Tytler, 1988; Caraveo et al., 1994) as sources of $25-25\fm5$. By the example of one of the most powerful [$\gamma$]{}–ray bursts — the short event GRB 790613 localized with the help of several space detectors with the best (in the northern sky) accuracy (Barat et al., 1984), whose localization error box has already been studied very well in the X–rays (see Greiner et al., 1995; and ROSAT X–ray Images, 1994a) and in the optical range (Ricker et al., 1986; Harrison et al., 1994; 