2016/03/17 by Aldo Batta, William H. Lee, Willaim H. Lee
Physics and Astronomy · #Accretion (finance) #Angular momentum #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Classical mechanics #Gamma-ray burst #Gamma-ray bursts and supernovae #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #Shutdown #Smoothed-particle hydrodynamics #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stw697
11 pages, 9 figures
arxiv created 2016/03/17 · openalex publication_date 2016/03/28 · arxiv updated 2016/04/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
For the collapsar scenario to be effective in the production of gamma ray bursts (GRBs), the infalling star's angular momentum J(r) must be larger than the critical angular momentum needed to form an accretion disc around a black hole (BH), namely Jcrit = 2rgc for a Schwarzschild BH. By means of 3D smoothed particle hydrodynamics simulations, here we study the collapse and accretion on to BHs of spherical rotating envelopes, whose angular momentum distribution has transitions between supercritical (J > Jcrit) and subcritical (J < Jcrit) values. Contrary to results obtained in previous 2D hydrodynamical simulations, we find that a substantial amount of subcritical material fed to the accretion disc, lingers around long enough to contribute significantly to the energy loss rate. Increasing the amount of angular momentum in the subcritical material increases the time spent at the accretion disc, and only when the bulk of this subcritical material is accreted before it is replenished by a massive outermost supercritical shell, the inner engine experiences a shutdown. Once the muffled accretion disc is provided again with enough supercritical material, the shutdown will be over and a quiescent time in the long GRB produced afterwards could be observed.