2003/01/01 by K. Nomoto, Ken'ichi Nomoto, Keiichi Maeda +10 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1143/ptps.151.44
published as Prog.Theor.Phys.Suppl.151:44-53,2003 · 12 pages, 9 figures. To appear in "Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003, eds. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories)
openalex publication_date 2003/01/01 · arxiv created 2003/06/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
Stars more massive than ∼ 20 – 25 M⊙ form a black hole at the end of their evolution. Stars with non-rotating black holes are likely to collapse “quietly" ejecting a small amount of heavy elements (Faint supernovae). In contrast, stars with rotating black holes are likely to give rise to very energetic supernovae (Hypernovae). We present distinct nucleosynthesis features of these two types of “black-hole-forming" supernovae. Nucleosynthesis in Hypernovae are characterized by larger abundance ratios (Zn,Co,V,Ti)/Fe and smaller (Mn,Cr)/Fe, which can explain the observed trend of these ratios in extremely metal-poor stars. Nucleosynthesis in Faint supernovae is characterized by a large amount of fall-back. We show that the abundance pattern of the recently discovered most Fe deficient star, HE0107-5240, and other extremely metal-poor carbon-rich stars are in good accord with those of black-hole-forming supernovae, but not pair-instability supernovae. This suggests that black-hole-forming supernovae made important contributions to the early Galactic (and cosmic) chemical evolution. Finally we discuss the nature of First (Pop III) Stars.