TY - GEN
T1 - Nucleosynthesis in core-collapse supernovae and GRB-metal-poor star connection
AU - Nomoto, K.
AU - Tominaga, N.
AU - Tanaka, M.
AU - Maeda, K.
AU - Umeda, H.
PY - 2007
Y1 - 2007
N2 - 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.
AB - 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.
KW - Gamma rays: bursts
KW - Nuclear reactions, nucleosynthesis, abundances
KW - Stars: Population II
KW - Stars: abundances
KW - Supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=36849046647&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=36849046647&partnerID=8YFLogxK
U2 - 10.1063/1.2803601
DO - 10.1063/1.2803601
M3 - Conference contribution
AN - SCOPUS:36849046647
SN - 0735404488
SN - 9780735404489
T3 - AIP Conference Proceedings
SP - 412
EP - 426
BT - SUPERNOVA 1987A
T2 - SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters
Y2 - 19 February 2007 through 23 February 2007
ER -