NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with Mzams = 1 to 25Msun and Z = 0.0001 to 0.02

摘要

We provide here a significant extension of the NuGrid Set 1 models in masscoverage and toward lower metallicity, adopting the same physics assumptions.The combined data set now includes the initial masses M/Msun = 1, 1.65, 2, 3,4, 5, 6, 7, 12, 15, 20, 25 for Z = 0.02, 0.01, 0.006, 0.001, 0.0001 withalpha-enhanced composition for the lowest three metallicities. These models arecomputed with the MESA stellar evolution code and are evolved up to the AGB,the white dwarf stage, or until core collapse. The nucleosynthesis wascalculated for all isotopes in post-processing with the NuGrid mppnp code.Explosive nucleosynthesis is based on semi-analytic 1D shock models.Metallicity-dependent mass loss, convective boundary mixing in low- andintermediate mass models and H and He core burning massive star models isincluded. Convective O-C shell mergers in some stellar models lead to thestrong production of odd-Z elements P, Cl, K and Sc. In AGB models with hotdredge-up the convective boundary mixing efficiency is reduced to accommodatefor its energetic feedback. In both low-mass and massive star models at thelowest metallicity H-ingestion events are observed and lead to i-processnucleosynthesis and substantial N-15 production. Complete yield data tables,derived data products and online analytic data access are provided.