2012/03/31 by Shunsaku Horiuchi, Kohta Murase, Kunihito Ioka +2 · 3 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #COSMIC cancer database #Cosmic ray #Gamma-ray burst #Gamma-ray bursts and supernovae #Hypernova #Jet (fluid) #Neutrino Physics Research #Range (aeronautics) #Supernova #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/753/1/69
published as Astrophys.J.753:69,2012 · v2 (16 pages, 7 figures, 1 table) matches published version (extended discussions, table added, conclusions unchanged)
arxiv created 2012/05/19 · openalex publication_date 2012/06/14 · arxiv updated 2015/04/23 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Heavy nuclei such as nickel-56 are synthesized in a wide range of core-collapse supernovae (CCSN), including energetic supernovae associated with gamma-ray bursts (GRBs). Recent studies suggest that jet-like outflows are a common feature of CCSN. These outflows may entrain synthesized nuclei at launch or during propagation, and provide interesting multi-messenger signals including heavy ultra-high-energy cosmic rays. Here, we investigate the destruction processes of nuclei during crossing from the stellar material into the jet material via a cocoon, and during propagation after being successfully loaded into the jet. We find that nuclei can survive for a range of jet parameters because collisional cooling is faster than spallation. While canonical high-luminosity GRB jets may contain nuclei, magnetic-dominated models or low-luminosity jets with small bulk Lorentz factors are more favorable for having a significant heavy nuclei component.