2018/01/31 by Takami Kuroda, Kei Kotake, Tomoya Takiwaki +2 · 98 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Black hole (networking) #Context (archaeology) #Gamma-ray bursts and supernovae #Gravitational collapse #Neutrino #Neutron star #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #Solar mass #Star (game theory) #Star formation #Stars #astro-ph.HE
paper · pdf · doi:10.1093/mnrasl/sly059
published in Monthly Notices of the Royal Astronomical Society Letters 477(1), L80-L84 (Oxford University Press) · 5 pages, 4 figures, accepted for publication in MNRAS letter
openalex created_date 2018/01/12 · arxiv created 2018/04/04 · openalex publication_date 2018/04/09 · arxiv updated 2018/05/16 · openalex updated_date 2026/08/05
Abstract We study the final fate of a very massive star by performing full general relativistic (GR), three-dimensional (3D) simulation with three-flavour multi-energy neutrino transport. Utilizing a 70 solar mass zero-metallicity progenitor, we self-consistently follow the radiation-hydrodynamics from the onset of gravitational core-collapse until the second collapse of the proto-neutron star (PNS), leading to black hole (BH) formation. Our results show that the BH formation occurs at a post-bounce time of Tpb ∼ 300 ms for the 70 M⊙ star. This is significantly earlier than those in the literature where lower mass progenitors were employed. At a few ∼10 ms before BH formation, we find that the stalled bounce shock is revived by intense neutrino heating from the very hot PNS, which is aided by violent convection behind the shock. In the context of 3D-GR core-collapse modelling with multi-energy neutrino transport, our numerical results present the first evidence to validate a fallback BH formation scenario of the 70 M⊙ star.