Evolution and Nucleosynthesis of Metal-free Massive Stars

We calculate presupernova evolutions and supernova explosions of massive stars (M = 13 − 25M⊙) for various metallicities. We find the following characteristic abundance patterns of nucleosynthesis in the metal-free (Pop III) stars. (1) The α-nuclei (from C to Zn) are more efficiently produced than other isotopes, and the abundance pattern of α-nuclei can be similar to the solar abundance. In particular, near solar ratios of alpha elements/Fe might be a signature of Pop III which could produce a large amount of Fe. (2) The abundance ratios of odd Z to even Z elements such as Na/Mg and Al/Mg become smaller for lower metallicity. However, these ratios almost saturate below Z ∼ < 10 , and [Na, Al/Mg] ∼ −1 for Pop III and low metal Pop II nucleosynthesis. This result is consistent with abundance pattern of metal poor stars, in which these ratios also saturate around −1. We suggest that these stars with the lowest [Na/Mg] or [Al/Mg] may contain the abundance pattern of Pop III nucleosynthesis. (3) Metal poor stars show interesting trends in the ratios of [Cr, Mn, Co/Fe]. We discuss that these trends are not explained by the differences in metallicity, but by the relative thickness between the complete and the incomplete Si burning layers. Large [Co/Fe] and small [Cr, Mn/Fe] values found in the observations are explained if mass cut is deep or if matter is ejected from complete Si burning layer in a form of a jet or bullets. (4) We also find that primary N production occurs in the massive Pop III stars, because these stars have radiative H-rich envelopes so that the convective layer in the He-shell burning region can reach the H-rich region.