Nucleosynthesis in Core-Collapse Supernovae and GRB—Metal-Poor Star Connection

Abstract

We review the nucleosynthesis yields of core‐collapse supernovae (SNe) for various stellar masses, explosion energies, and metallicities. Comparison with the abundance patterns of metalpoor stars provides excellent opportunities to test the explosion models and their nucleosynthesis. We show that the abundance patterns of extremely metal‐poor (EMP) stars, e.g., the excess of C, Co, Zn relative to Fe, are in better agreement with the yields of hyper‐energetic explosions (Hypernovae, HNe) rather than normal supernovae.We note that the variation of the abundance patterns of EMP stars are related to the diversity of the Supernova‐GRB connection. We summarize the diverse properties of (1) GRB‐SNe, (2) Non‐GRB HNe/SNe, (3) XRF‐SN, and (4) Non‐SN ORB. In particular, the Non‐SN GRBs (dark hypernovae) have been predicted in order to explain the origin of C‐rich EMP stars. We show that these variations and the connection can be modeled in a unified manner with the explosions induced by relativistic jets. Finally, we examine whether the most luminous supernova 2006gy can be consistently explained with the pair‐instability supernova model.