1.05 & 20.81 & 37.0\
01:14 & c B & 600 & 1.30 & 22.62 & 39.0\
00:30 & c V & 600 & 1.20 & 21.50 & 38.8\
00:55 & c R & 600 & 1.18 & 20.63 & 38.0\
00:41 & c R & 600 & 1.14 & 20.60 & 38.5\

Search strategy
===============

Let us assume that what we are looking for in the [$\gamma$]{}–ray box under investigation is indeed a single compact object of neutron star type. For example, it could be an object partially or totally consisting of quark matter, which has been a hypothesis so far (Haensel et al., 1986; Overgard & Ostgaard, 1991). But here we try to formulate a possible observational forecast without any theoretical model describing [$\gamma$]{}–ray burst by itself. We do not assume any particular burst model in advance. The only thing which can be now investigated from observations is the compact character of their sources. Although till now the validity of absorption (cyclotron?) features in redshifted annihilation lines observed in the spectra of “old” [$\gamma$]{}–ray bursts is disputed and carefully tested, the observational fact of fast temporal flux variations in bursts is not in question (Atteia et al., 1987; 