2006MNRAS.367L..42P

We use the available radio, optical and X-ray measurements for the afterglows of the short bursts 050709 and 050724 to constrain the blast-wave energy, its collimation and the density of the circumburst medium. For GRB 050709 (the duration of which was 0.07 s), we identify two kinds of models: (i) a high-density solution, where the ejecta are collimated in a jet of half-angle θ_jet> 6° and interact with a medium of particle density 10^–4 < n < 0.1/cm3; and (ii) a low-density solution with θ_jet > 2° and n < 10^–5/cm3. These density ranges are compatible with those expected in the vicinity of the host galaxy and in the intergalactic medium, lending support to the hypothesis that the progenitor of GRB 050709 is a neutron star-neutron star or neutron star-black hole merger. For GRB 050724 (which lasted 1.5 s), we obtain 0.1 < n < 10³/cm3 and θ_jet > 8°. The range of allowed densities shows that this burst occurred in the interstellar medium. The dynamical parameters of the high-density model for the GRB afterglow 050709 are similar to those for 050724. If these parameters are representative for short-GRB outflows, then these jets are less collimated and have a lower kinetic energy than those of long bursts, which suggests that GRB jets are not magnetically collimated and are powered by the gravitational energy of the torus. Evidently, the analysis of more short-GRB afterglows is required for a more robust conclusion.