Explosive Nucleosynthesis in GRB Jets Accompanied by Hypernovae

• Published in: The Astrophysical journal Vol. 647; no. 2; pp. 1255 - 1268
• Main Authors: Nagataki, Shigehiro, Mizuta, Akira, Sato, Katsuhiko
• Format: Journal Article
• Language: English
• Published: Chicago, IL IOP Publishing 20.08.2006; University of Chicago Press
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; Galaxy halo; nuclear reactions, nucleosynthesis, abundances; Cosmic gamma sources; Black holes; accretion, accretion disks; Nucleosynthesis; Abundance; Gamma ray burst; Accretion disks; supemovae: general; Galaxy: halo; black hole physics; Cosmology; Jets; gamma rays: bursts
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/505618

Two-dimensional hydrodynamic simulations are performed to investigate explosive nucleosynthesis in a collapsar using the model of MacFadyen and Woosley. It is shown that super(56)Ni is not produced in the jet of the collapsar sufficiently to explain the observed amount in a hvpernova when the duration of the explosion is 610 s. Even though a considerable amount of super(56)Ni is synthesized if all the explosion energy is deposited initially, the opening angles of the jets become too wide to realize highly relativistic outflows. From these results, it is concluded that the origin of super(56)Ni in hypernovae associated with GRBs is not the explosive nucleosynthesis in the jet. We consider that the idea that the origin is the explosive nucleosynthesis in the accretion disk is more promising. We also show that the explosion becomes bipolar naturally because of the deformed progenitor. This fact suggests that the super(56)Ni is synthesized in the accretion disk and conveyed as outflows blown along the rotation axis, which will explain the line features of SN 1998bw and the double-peaked line features of SN 2003jd. Some fraction of the gamma-ray lines from super(56)Ni decay in the jet will appear without losing their energies as long as the jet is a relativistic flow, which may be observed as relativistically Lorentz-boosted line profiles in the future. We show that the abundance of nuclei whose mass number 640 in the ejecta depends sensitively on the energy deposition rate. So it may be determined by observations of chemical composition in metal-poor stars which model is the proper one.