Find out in which region of the star, and by which hydrostatic or explosive burning, each isotope is produced. The ejecta are split into the wind, the hydrostatic burning zones of the pre-supernova star and the explosive burning zones, and the yield of every isotope is attributed to them.
To follow one isotope or element across all masses, metallicities and rotations, use the production across the grid page.
Limongi & Chieffi 2018 · ApJS 237, 13
Model
One model at a time
Zone structure
Mass coordinate on a logarithmic scale above the mass cut. The hydrostatic zones come from the pre-explosive structure; the explosive zones are bounded by the radii where the peak temperature of the shock drops below 5, 4, 3.3 and 1.9 × 109 K. The two sets overlap: for each isotope the yield above the point where the explosion starts to modify it is attributed to the hydrostatic zones, the rest to the explosive ones.
Chart of the nuclides
Click an isotope to analyse it
Selected isotope
Share of the production per zone
Mass fraction (green/violet) and its cumulative from the surface (blue, right axis): before (dashed) and after (solid) the explosion
All isotopes
Percentage of the production of each isotope in each zone
How it works
Zones. The wind is the mass lost before the explosion. The hydrostatic zones are located in the pre-supernova structure: H burning (until X(H) < 10−8), He shell (X(He) < 10−2), the former convective He core, C shell (X(12C) < 10−3), Ne shell (X(12C) and X(20Ne) < 10−3) and the O-burning zone down to the mass cut. The explosive zones are bounded by the pre-explosive radii where the peak temperature of the shock falls below 5, 4, 3.3 and 1.9 × 109 K: complete and incomplete explosive Si burning, explosive O burning and explosive C/Ne burning.
Attribution. A species is considered produced if its yield exceeds 1.05 times its initial abundance in the ejecta (production factor). The cumulative yield of the exploded model (unstable species decayed) is split among the zones. Where pre- and post-explosive profiles differ, the yield above that point is given to the hydrostatic zones and the yield below it to the explosive zones. In the hydrostatic zones the material is then redistributed where the abundance profile is flat (He core and shell are fused for 4He, and O shell, Ne shell and C shell for 16O), and the part present in the initial envelope is discarded: only the production is shown.
Class. An isotope is "explosive" if more than 67% of its production comes from the explosive zones, "hydrostatic" if more than 67% comes from the hydrostatic zones, "mixed" otherwise. The "main production zone" in the chart merges the wind with H burning and the He core with the He shell.
Sets. F: 0.07 M☉ of 56Ni, no mixing; I: as F but M > 25 M☉ collapse (only the wind is ejected); M: mixing and fall-back (inner border [Ni/Fe] = 0.2, outer border at the base of the O shell, X(O) = 0.001) and mass cut re-chosen for 0.07 M☉ of 56Ni; R: as M but M > 25 M☉ collapse. "Custom" lets you choose the mixing parameters, the collapse mass and either the ejected 56Ni or the mass cut. Net excess. By default the explosive zones are credited only with what the explosion adds to the pre-explosive abundance (the points where the cumulative curve rises more steeply); the rest of the final profile is attributed to the hydrostatic zone it comes from. "As in prosit.f90" credits the explosive zones with the whole post-explosive profile below the point where the explosion starts to act. Mass cut. Only the models with an exploded profile are available (the most massive models collapse directly into a black hole).
Computed locally in your browser from Exploded_Models/*exp.chi, *ini.chi, *tmax.txt and wind_profiles/*pub.wnd. The page must be served over http(s) (e.g. python3 -m http.server in the website folder).