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We calculate evolution, collapse, explosion, and nucleosynthesis ofPopulation III very-massive stars with 500$M_{\odot}$ and 1000$M_{\odot}$.Presupernova evolution is calculated in spherical symmetry. Collapse andexplosion are calculated by a two-dimensional code, based on the bipolar jetmodels. We compare the results of nucleosynthesis with the abundance patternsof intracluster matter, hot gases in M82, and extremely metal-poor stars in theGalactic halo. It was found that both 500$M_{\odot}$ and 1000$M_{\odot}$ modelsenter the region of pair-instability but continue to undergo core collapse. Inthe presupernova stage, silicon burning regions occupy a large fraction, morethan 20% of the total mass. For moderately aspherical explosions, the patternsof nucleosynthesis match the observational data of both intracluster medium andM82. Our results suggest that explosions of Population III core-collapsevery-massive stars contribute significantly to the chemical evolution of gasesin clusters of galaxies. For Galactic halo stars, our [O/Fe] ratios are smallerthan the observational abundances. However, our proposed scenario is naturallyconsistent with this outcome. The final black hole masses are $\sim230M_{\odot}$ and $\sim 500M_{\odot}$ for the $500M_{\odot}$ and1000$M_{\odot}$ models, respectively. This result may support the view thatPopulation III very massive stars are responsible for the origin ofintermediate mass black holes which were recently reported to be discovered.Comment: 49 pages, 49 figure files, accepted to ApJ (2006, 645, 2

Core‐Collapse Very Massive Stars: Evolution, Explosion, and Nucleosynthesis of Population III 500–1000M⊙Stars

Core‐Collapse Very Massive Stars: Evolution, Explosion, and Nucleosynthesis of Population III 500–1000M_⊙Stars