2002/05/22 by Hideyuki Umeda, Ken'ichi Nomoto, K. Nomoto +2
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0205365
4 pages, 4 Fig, in Proc. 11th Workshop on Nuclear Astrophysics, p.164, ed. W. Hillebrand & E. Muller (Max-Planck-Institut fur Astrophysik), Ringberg Castle, Germany, 2/11-16, 2002
arxiv created 2002/05/22 · openalex publication_date 2002/05/22 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We calculate evolution and nucleosynthesis in massive Pop III stars with M = 13 ~ 270Msun, and compare the results with abundances of very metal-poor halo stars. The observed abundances can be explained by the energetic core-collapse supernovae with M < ~ 130Msun (``hypernovae'') but not by pair-instability supernovae (PISNe) with M ~ 140-270 Msun. This result constrain the IMF for the Pop III and very metal-poor Pop II stars.