2018/05/30 by J. J. Grimmett, J J Grimmett, Alexander Heger +3 · 16 citations
Physics and Astronomy · #Astrophysics #Energy (signal processing) #Gamma-ray bursts and supernovae #Hypernova #Nucleosynthesis #Physics #Population #Pulsars and Gravitational Waves Research #Star (game theory) #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph.HE
paper · pdf · doi:10.1093/mnras/sty1417
published in Monthly Notices of the Royal Astronomical Society (Oxford University Press)
arxiv created 2018/05/30 · openalex publication_date 2018/05/30 · arxiv updated 2018/06/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the relationship between explosion energy and nucleosynthesis in Population III supernovae and provide nucleosynthetic results for the explosions of stars with progenitor masses of 15 M⊙, 20 M⊙, 30 M⊙, 40 M⊙, 60 M⊙, and 80 M⊙, and explosion energies between approximately 1050 erg and 1053 erg. We find that the typical abundance pattern observed in metal-poor stars is best matched by supernovae with progenitor mass in the range 15 M⊙– 30 M⊙ and explosion energy of ∼(5−10) × 1051 erg. In these models, a reverse shock caused by jumps in density between shells of different composition serves to decrease synthesis of chromium and manganese, which is favourable to matching the observed abundances in metal-poor stars. Spherically symmetric explosions of our models with progenitor mass ≥40 M⊙ do not provide yields that are compatible with the iron-peak abundances that are typically observed in metal-poor stars; however, by approximating the yields that we might expect from these models in highly aspherical explosions, we find indications that explosions of stars 40 M⊙ – 80 M⊙ with bipolar jets may be good candidates for the enrichment sources of metal-poor stars with enhanced carbon abundances.