Population III Core-Collapse Supernova Yields and Extremely Metal-Poor Star Abundance Pattern

摘要

Recently, very accurate observations of abundances of extremely metal-poor (EMP) stars have been performed with VLT and SUBARU. They determined Vhe abundance patterns of many EMP stars with ~4'2 [Fe/H] ~2. In the result, it is confirmed with small dispersions that the abundance ratios of these stars are obtained as a function of the metallicity. For example, the EMP stars with smaller [Fe/H] have larger [Zn,Co/Fe] and smaller [Cr/Fe]. Therefore Cayrcl et al. Q004) and Francois et al. (2004) suggested homogeneous mixing in the Galaxy even below [Fe/H]~ 3, although this conflicts with the Galactic chemical evolution models. We calculate explosions and nucleosynthesis of population III supernovae (SNe) with mixing-fallback model (Umeda & Nomoto 2003; 2005; Tominaga et al. 2006) and show that the trends of the abundance ratios with the small dispersions can be understood by the variations of explosion energies and progenitors' masses in inhomogeneous mixing.