Models Used in Existing Hydrocodes

gasoline2/ChaNGa

Feedback from core collapse SN is governed based on a choice of IMF and stellar lifetimes derived from Equation 3 of Raiteri 1996.

These lifetimes depend on the mass M and metallicity Z of the star (in solar units) and are given by:

\[t_*(\mathrm{yr}) = a_0(Z) + a_1(Z)\log(M) + a_2(Z)(\log(M))^2\]

With the metallicity-dependent coefficients a_i(Z) given by:

\[\begin{split}\begin{aligned} a_0(Z) &= 10.13 + 0.07547\log(Z) - 0.008084\left(\log(Z)\right)^2 \\ a_1(Z) &= -4.424 - 0.7939\log(Z) - 0.1187\left(\log(Z)\right)^2 \\ a_2(Z) &= 1.262 + 0.3385\log(Z) + 0.05417\left(\log(Z)\right)^2 \end{aligned}\end{split}\]