2018MNRAS.479..495G

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) x 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.