NuGrid stellar data set I. Stellar yields from H to Bi for stars with metallicities Z = 0.02 and Z = 0.01

摘要

We provide a set of stellar evolution and nucleosynthesis calculations thatapplies established physics assumptions simultaneously to low- andintermediate-mass and massive star models. Our goal is to provide an internallyconsistent and comprehensive nuclear production and yield data base forapplications in areas such as pre-solar grain studies. Our non-rotating modelsassume convective boundary mixing where it has been adopted before. We include8 (12) initial masses for $Z = 0.01$ ($0.02$). Models are followed either untilthe end of the asymptotic giant branch phase or the end of Si burning,complemented by a simple analytic core-collapse supernova models with twooptions for fallback and shock velocities. The explosions show whichpre-supernova yields will most strongly be effected by the explosivenucleosynthesis. We discuss how these two explosion parameters impacts thelight elements and the $s$ and $p$ process. For low- and intermediate-massmodels our stellar yields from H to Bi include the effect of convectiveboundary mixing at the He-intershell boundaries and the stellar evolutionfeedback of the mixing process that produces the $^{13}$C pocket. Allpost-processing nucleosynthesis calculations use the same nuclear reaction ratenetwork and nuclear physics input. We provide a discussion of the nuclearproduction across the entire mass range organized by element group. All ourstellar nucleosynthesis profile and time evolution output is availableelectronically, and tools to explore the data on the NuGrid VOspace hosted bythe Canadian Astronomical Data Centre are introduced.