2005/11/18 by A. Panaitescu · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2005.00134.x
published as Mon.Not.Roy.Astron.Soc.Lett.367:L42-L46,2006 · 5 pages, submitted to MNRAS
arxiv created 2005/11/18 · openalex publication_date 2006/01/31 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Abstract 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 θjet > 6° and interact with a medium of particle density 10−4 < n < 0.1 cm−3; and (ii) a low-density solution with θjet > 2° and n < 10−5 cm−3. 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 cm−3 and θjet > 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.