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

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

2007-07-15

arxiv.org/abs/0707.2187v1

AIP Conf.Proc.937:412-426,2007

Astronomy and Astrophysics

Astrophysics

15 pages, 9 figures. To appear in "Supernova 1987A: 20 Years After: Supernovae and Gamma-Ray Bursters", eds. S. Immler, K. Wei

Scientific paper

10.1063/1.2803601

We review the nucleosynthesis yields of core-collapse supernovae (SNe) for various stellar masses, explosion energies, and metallicities. Comparison with the abundance patterns of metal-poor 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 GRB. 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.

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