Nucleosynthesis in Massive Core-Collapse Supernovae as the Origin of Abundances in Extremely Metal-Poor Stars

Details Nucleosynthesis in Massive Core-Collapse Supernovae as the Origin of Abundances in Extremely Metal-Poor Stars Nucleosynthesis in Massive Core-Collapse Supernovae as the Origin of Abundances in Extremely Metal-Poor Stars

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..163u&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astronomy

Scientific paper

We calculate nucleosynthesis in Population (Pop) III supernovae (SNe) and compare the yields with various abundance patterns of extremely metal-poor (EMP) stars. We assume that the observed EMP stars are the second generation stars, which have the metal-abundance pattern of the Pop III SNe. Previous theoretical yields and observations do not match well, suggesting that the simplest supernova model cannot account for the observations. In this paper we consider high energy explosions, "low-density" explosions, and mixing-fallback models. We show that the abundance patterns of both C-normal and C-rich EMP stars with [Fe/H] ≲ - 2.5 can be well reproduced with the yield of core-collapse SNe of M ~ 20 - 130M&sun;. The abundance patterns of the [Fe/H] ~ -2.5 stars correspond to supernova yields with normal explosion energies, while those of the C-normal ([C/Fe] < 1) stars with [Fe/H] ≃ -4 ~ -3 correspond to high-energy supernova yields. The abundance pattern of C-rich [C/Fe] ≳ 2) low [Fe/H] (≃ - 5 ~ - 3.5) stars can be explained with the faint SN yield with little 56Ni ejection, which is similar to SN1997D. Even we vary parameters, we still need a large explosion energy to obtain the large Co/Fe and Zn/Fe ratios observed in typical EMP stars.

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