Nucleosynthetic yields - 2025 grid (Limongi et al. 2025, ApJS, 279, 41)

Content of this directory

Yields of the explosive models for the following grid:

Initial Masses (Solar Masses)     : 9.22, 10, 11, 12, 13, 15
Initial Metallicity [Fe/H]        : 0
Initial Rotation Velocity (km/s)  : 0 (non rotating)

There are yields for 2 different choices of the mass cut (the mass coordinate that separates the
remnant from the ejecta), each one stored in its own sub-directory:

Ni-Burrows : the mass cut is fixed by assuming the initial mass - ejected 56Ni mass relation
             obtained by Burrows et al. (2024) from full 3D hydrodynamical simulations, i.e. the
             ejected 56Ni mass (in Msun) is
                  9.22 Msun -> 1.04e-2     10 Msun -> 1.95e-2     11 Msun -> 2.92e-2
                  12   Msun -> 3.55e-2     13 Msun -> 4.17e-2     15 Msun -> 5.42e-2
Ni-007     : the mass cut is fixed by requiring the ejection of 0.07 Msun of 56Ni for all the masses.
             Note that in the 9.22 Msun model the maximum amount of 56Ni that can be ejected is
             about 0.048 Msun, which is the value reported in the corresponding file.

For each initial mass and for each mass cut there are 3 files, named "mmmmzvvv.ext":

mmmm = initial mass in units of 0.01 Msun (i.e. '0922' means 9.22 Msun, '1000' means 10 Msun)
z    = initial metallicity ('a' = [Fe/H] = 0)
vvv  = initial equatorial rotational velocity in km/s ('000' = non rotating)
ext  = type of yields:

   yiso_nod  = isotopic yields in which the unstable nuclei are NOT fully decayed (they are
               allowed to decay only for a short time after the explosion). It contains
               338 species, including free neutrons (N), protons (P) and alpha particles (A).
               Note that P and A must be summed to H and He4, i.e. H+P and He4+A are the
               correct abundances of H and He4.
   yiso_dec  = isotopic yields in which all the unstable nuclei are forced to fully decay to
               their closest stable daughter. It contains 142 stable isotopes.
   yele_dec  = elemental yields obtained after the full decay of all the unstable nuclei
               (sum over the stable isotopes of each element). It contains 53 elements.

Format of the files

Each file is a plain ASCII table. The first row contains the column labels, each of the
following rows refers to one species. The columns are:

nome     =  name of the species (isotope, e.g. 'Fe56', or element, e.g. 'Fe')
Z        =  atomic number
A        =  mass number (0 in the elemental files)
initial  =  initial abundance of the species in the star, in mass fraction
PF       =  production factor, i.e. the ratio between the mean mass fraction of the species in the
            ejecta (total yield / total ejected mass) and its initial mass fraction.
            Species that are not present initially have PF = 1e-30
YieldTot =  total yield, i.e. the mass (in solar masses) of the species ejected by the star
            (wind + explosion)
NewProd  =  net yield (in solar masses), i.e. the total yield minus the amount of the species
            that was originally present in the ejected mass (it is negative for the species
            that are destroyed, e.g. H)
solari   =  initial (scaled solar) abundance of the species, in mass fraction. It is the same
            as the column 'initial'
wind     =  contribution of the stellar wind to the total yield, in solar masses

Note: all the yields are in solar masses.