Mass loss over time
Wind mass-loss histories for the model grid.
2018 model grid · massive stars
Stellar models at different metallicities
Rotating and non-rotating stellar models with evolutionary properties, pre-supernova structures, nucleosynthetic yields, and remnant masses.
Published · ApJS 237, 13 (2018)
Model grid
Nine initial masses · four metallicities · three rotation velocities
Initial masses: 13, 15, 20, 25, 30, 40, 60, 80, and 120 M☉. Initial metallicities: [Fe/H] = 0, −1, −2, and −3. Initial rotation velocities: 0, 150, and 300 km s−1.
Evolutionary and pre-supernova data
Choose a dataset, then download the metallicity set you need.
Evolutionary properties
Time-dependent stellar properties, central abundances, and core-collapse quantities.
Pre-supernova structures
Physical profiles and chemical composition at the pre-supernova stage.
Nucleosynthetic yields
Four explosion and fallback prescriptions.
For the yield definitions, file naming conventions, and integrated-yield tables, see the yield data guide.
Want a different prescription? Use the interactive yields calculator to choose the mass cut or 56Ni, mixing and fall-back, and the direct-collapse mass.
Where is each isotope produced? Use the isotope origin explorer to see which hydrostatic and explosive burning zones synthesize it, or the production across the grid to follow an isotope or element over all masses, [Fe/H] and rotations.
Set F · fixed 56Ni
Each model ejects 0.07 M☉ of 56Ni.
Set I · direct collapse
For models above 25 M☉, the star collapses into the remnant and only the wind is ejected.
Set M · mixing and fallback
Mixing and fallback boundaries are applied before setting the mass cut to eject 0.07 M☉ of 56Ni.
Set R · fallback and direct collapse
Uses the Set M prescription up to 25 M☉; above that mass, only the wind is ejected.
Additional datasets
Selected pre-supernova properties
Selected physical quantities at the pre-supernova stage.
Remnant masses
Remnant mass values for the published model grid.
Reference
If you use these data, please cite Limongi, M. & Chieffi, A. 2018, The Astrophysical Journal Supplement Series, 237, 13.