Models included

In order to estimate an age for a white dwarf a chain of models have to be used. Here are the models included in \(\texttt{wdwarfdate}\).

\(\texttt{wdwarfdate}\)

Models Included

Cooling Models

Cooling tracks from the Montreal White Dwarf Group available online (Berdard et al. 2020):
  • Thick H layer (DA)

  • Thin H layer (non-DA)

IFMR

Stellar evolution models

MESA Isochrones available online (Choi et al. 2016 and Dotter 2016):
  • \([{\rm Fe/H}] = -4.00, -1.00, 0.00, 0.50\)

  • \({\rm v/vcrit} = 0.0, 0.4\)

  • \([\alpha/{\rm Fe}] = 0\)

Constraints

We summarize here the most important constraints when using \(\texttt{wdwarfdate}\). For a complete discussion see Kiman et al. 2022.

  • Combining the limitation of the cooling tracks with the restrictions of the IFMR, the values for which \(\texttt{wdwarfdate}\) can estimate a total age are \(1,500 \lesssim T_{\rm eff} \lesssim 90,000\,{\rm K}\) and \(7.9 \lesssim \log g \lesssim 9.3\).

  • Given that the cooling tracks assume single star evolution and C/O core for the white dwarfs, the best range of final masses to use \(\texttt{wdwarfdate}\) is \(0.45-1.1\,{\rm M}_{\odot}\), because outside this range objects are not likely to have evolved as a single star.