2005/02/28 by Kazunori Kohri, Ramesh Narayan, Tsvi Piran
Physics and Astronomy · #Astrophysics and Star Formation Studies #Gamma-ray bursts and supernovae #Neutrino Physics Research #astro-ph #hep-ph
paper · pdf · doi:10.1086/431354
published as Astrophys.J. 629 (2005) 341-361 · 53 pages, 14 figures, to appear in ApJ
arxiv created 2005/04/25 · openalex publication_date 2005/08/03 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We suggest that part of the infalling material during the core collapse of a massive star goes into orbit around the compact core to form a hot, dense, centrifugally supported accretion disk whose evolution is strongly influenced by neutrino interactions. Under a wide range of conditions, this neutrino-dominated accretion flow will be advection dominated and will develop a substantial outflowing wind. We estimate the energy carried out in the wind and find that it exceeds 10 50 ergs for a wide range of parameters and even exceeds 10 51 ergs for reasonable parameter choices. We propose that the wind energy will revive a stalled shock and will help produce a successful supernova explosion. We discuss the role of the disk wind in both prompt and delayed explosions. While both scenarios are feasible, we suggest that a delayed explosion is more likely and perhaps even unavoidable. Finally, we suggest that the disk wind may be a natural site for r -process nucleosynthesis.