2013/01/25 by A. V. Penacchioni, Ana Virginia Penacchioni, Remo Ruffini +10
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Computer science #Context (archaeology) #Eclipse #Gamma-ray burst #Gamma-ray burst progenitors #Gamma-ray bursts and supernovae #Intermediate-mass black hole #Neutron star #Physics #Supernova #Swift #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1051/0004-6361/201220679
12 pages, 17 figures, to appear on A&A
arxiv created 2013/01/25 · openalex publication_date 2013/01/30 · arxiv updated 2015/06/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Context. Gamma-ray burst (GRB) 110709B is the first source for which Swift-BAT was triggered twice, with a time separation of ~10 min. The first emission (called here episode 1) lasted from 40 s before the first trigger time until 60 s after it. The second emission (hereafter episode 2) lasted from 35 s before the second trigger time until 100 s after it. These features reproduce those of GRB 090618, which has recently been interpreted within the induced gravitational collapse (IGC) paradigm. In line with this paradigm, we assume the progenitor to be a close binary system composed of the core of an evolved star and a neutron star (NS). The evolved star explodes as a supernova (SN) and ejects material that is partially accreted by the NS. We identify this process with episode 1. The accretion process accumulates more than the critical mass of the NS, which gravitationally collapses into a black hole (BH). This process leads to the GRB emission, episode 2. The two trigger episodes have for the first time provided the possibility to cover the X-ray emission observed by XRT both prior to and during the prompt phase of GRB 110709B.