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2018 model grid · interactive tool

Interactive yields calculator

Compute the yields of all the 2018 models (all masses, metallicities and rotations) by choosing the mass cut or the ejected 56Ni, whether to apply mixing and fall-back, and the mass above which the star collapses directly.

Limongi & Chieffi 2018 · ApJS 237, 13

Parameters

Applied to the whole grid: 9 masses × 4 [Fe/H] × 3 rotations

1 · Mass cut

2 · Mixing and fall-back

Outer border: first zone from the bottom where the elemental mass fraction of O exceeds the value. Inner border: going down from it, the zone free of O and Si where [X/Fe] of the (decayed) material above reaches the value. Between them the composition is homogenised; the mass cut is applied to the mixed profile and everything below the inner border is discarded.

3 · Direct collapse

Models with an initial mass above this value collapse entirely into the remnant: only the wind is ejected.

Model files

Advanced: load the model files manually

Only needed if the page is opened from disk instead of the website. Select all the *exp.chi and *pub.wnd files together; they are matched by name.

How it works

Logic. The post-explosion profile is read (the innermost Fe-core zone is dropped if it contains no H and He) and the wind is appended as the last zone [Mfin, Mini]. Unstable isotopes decay instantly onto their daughter (network.txt); element tables and cumulative yields from the surface inward are built from the decayed composition. Mixing and fall-back. The outer border is the first zone, from the bottom, where X(O) exceeds the chosen value (0.1); the inner border is searched downward from it among the zones with X(O) and X(Si) < 10−3, where [X/Fe] of the material above (solar: Asplund et al. 2009) exceeds the chosen value (e.g. [Ni/Fe] = 0.2), with the partial zone interpolated. The zones in between are replaced by their mass-weighted mean; everything below the inner border falls back. All models. The same parameters are applied to every model of the grid; columns are labelled mmmzvvv (mass, [Fe/H] a=0, b=−1, c=−2, d=−3, rotation in km/s). Mass cut. For a requested 56Ni, the first zone from the surface whose cumulative (undecayed) 56Ni exceeds the target is found; mass cut and cumulative yields are linearly interpolated inside it (constant composition). For a fixed mass cut, the same interpolation is used. Yields. Total yield = ejected mass above the cut, wind included; "Explosion" is the total minus the wind. Above the direct-collapse mass only the wind is ejected. Net = total − initial composition × (Mini − mass cut), with the initial composition rescaled to the Z and Y of the chosen [Fe/H]; PF = total / (initial composition × (Mini − mass cut)), i.e. relative to the star's own initial abundances (equal to solar for [Fe/H] = 0). Values in M☉.
Computed locally in your browser. The page must be served over http(s); if opened from disk (file://) the data cannot be loaded automatically — use the manual file loader to select all the *exp.chi files (from Exploded_Models/) and *pub.wnd files (from wind_profiles/) together, or run python3 -m http.server in this folder.