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Supernova Nucleosynthesis in the early universe

Published online by Cambridge University Press:  01 June 2008

Nozomu Tominaga
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo, Japan email: nozomu.tominaga@nao.ac.jp
Hideyuki Umeda
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo, Japan
Keiichi Maeda
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba, Japan
Ken'ichi Nomoto
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo, Japan Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba, Japan
Nobuyuki Iwamoto
Affiliation:
Nuclear Data Center, Nuclear Science and Engineering Directorate, Japan Atomic Energy Agency, Tokai, Ibaraki, Japan
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Abstract

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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 [Ėdep = (0.3 − 1500) × 1051 ergs s−1], and (2) SNe of stars with various main-sequence masses (Mms = 13 − 50M) and explosion energies [E = (1 − 40) × 1051ergs]. 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].

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

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