We provide our first set of stellar evolution sequences and nucleosynthesis calculations for low-mass , intermediate-mass and massive stars ( Set 1 in NuGrid data production hereafter ) .
Set 1 uses “ baseline ” physics assumptions for stellar models , which are 1D spherical symmetry , no rotation or magnetic fields and conservative assumptions for convective boundary mixing .
Stellar data is provided for initial masses M / M _ { \odot } = 1.5 , 3 , 5 , 15 , 20 , 25 , 32 , and 60 for a metallicity of Z = 0.02 and for M / M _ { \odot } = 1.5 , 3 , 5 , 15 , 20 , and 25 for Z = 0.01 .
Low- and intermediate-mass models ( M \leq 5 M _ { \odot } ) are computed until the end of the asymptotic giant branch ( AGB ) phase and the massive star models until the end of Si burning .
Explosive nucleosynthesis in core-collapse supernovae is simulated using one-dimensional analytic trajectories .
Post-processing calculations use the same nuclear reaction rates , providing an internally consistent set of yields and nucleosynthesis data for our entire mass range .
We provide the first grid of stellar yields from H to Bi for low- and intermediate-mass models that include diffusive convective boundary mixing at the He-intershell boundaries and s -process nucleosynthesis during the AGB phase .
For massive stars , Set 1 includes core-collapse supernovae models with fallback and high shock velocities We show the impact of these two variables on the light elements and on the s - and p-process .
Comparing the yields from the different models we find , e.g. , that intermediate-mass stars can significantly contribute to the production of oxygen in addition to massive stars .