2008/06/01 by Nozomu Tominaga, Hideyuki Umeda, Keiichi Maeda +3
Physics and Astronomy · #Abundance (ecology) #Astronomy #Astrophysics #Gamma-ray bursts and supernovae #Nucleosynthesis #Physics #Population #Pulsars and Gravitational Waves Research #Stars #Stellar nucleosynthesis #Stellar, planetary, and galactic studies #Supernova #Universe #astro-ph
paper · pdf · doi:10.1017/s1743921308024800
5 pages, 4 figures. To appear in "Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies", Proceedings of IAU Symposium 255 (June 2008, Rapallo), eds. L.K. Hunt, S. Madden, & R. Schneider (Cambridge Univ. Press)
openalex publication_date 2008/06/01 · arxiv created 2008/09/24 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract The first metal enrichment in the universe was made by supernova (SN) explosions of population (Pop) III stars. The history of chemical evolution is recorded in abundance patterns of extremely metal-poor (EMP) stars. We investigate the properties of nucleosynthesis in Pop III SNe by comparing their yields with the abundance patterns of the EMP stars. We focus on (1) jet-induced SNe with various properties of the jets, especially energy deposition rates [Ė dep = (0.3 − 1500) × 10 51 ergs s −1 ], and (2) SNe of stars with various main-sequence masses ( M ms = 13 − 50 M ⊙ ) and explosion energies [ E = (1 − 40) × 10 51 ergs]. The varieties of Pop III SNe can explain the observations of the EMP stars: (1) higher [C/Fe] for lower [Fe/H] and (2) trends of abundance ratios [X/Fe] against [Fe/H].