2006/07/14 by A. I. Bogomazov, А. И. Богомазов, V. Lipunov +3 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Compact star #Galaxy #Gamma-ray burst #Gamma-ray burst progenitors #Gamma-ray bursts and supernovae #Intermediate-mass black hole #Neutron star #Physics #Pulsars and Gravitational Waves Research #Spin-flip #Stars #Stellar black hole #White dwarf #astro-ph
paper · pdf · doi:10.1134/s1063772907040063
published as Astron.Rep.51:308-317,2007 · 18 pages, 3 figures
arxiv created 2006/07/14 · openalex publication_date 2007/04/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We analyze the late stages of evolution of massive (M 0 ≳ 8 M ⊙) close binaries, from the point of view of possible mechanisms for the generation of gamma-ray bursts. It is assumed that a gamma-ray burst requires the formation of a massive (∼1 M ⊙), compact (R ≲ 10 km) accretion disk around a Kerr black hole or neutron star. Such Kerr black holes are produced by core collapses of Wolf-Rayet stars in very close binaries, as well as by mergers of neutron stars and black holes or two neutron stars in binaries. The required accretion disks can also form around neutron stars that were formed via the collapse of ONeMg white dwarfs. We estimate the Galactic rate of events resulting in the formation of rapidly rotating relativistic objects. The computations were carried out using the “Scenario Machine.”