Non-equilibrium cooling rate for a collisionally cooled metal-enriched
  gas
  We present self-consistent calculations of non-equilibrium (time-dependent)
cooling rates for a dust-free collisionally controlled gas in wide temperature
($10 K\le T\le 10^8 K$) and metallicity ($10^{-4} Z_\odot \le Z \le 2 Z_\odot$)
ranges. We confirm that molecular hydrogen dominates cooling at $10^2 \simlt
T\simlt 10^4$ K and $Z\simlt 10^{-3} Z_\odot$. We find that the contribution
from H$_2$ into cooling rate around $T\sim (4-5)\times 10^3$ K stimulates
thermal instability in the metallicity range $Z\simlt 10^{-2} Z_\odot$.
Isobaric cooling rates are generally lower than isochoric ones, because the
associated increase of gas density leads to both more efficient hydrogen
recombination and equilibration of the fine-structure level populations.
Isochoric cooling keeps the ionization fraction remains quite high at
$T\simlt10^4$ K: up to $\sim0.01$ at $T\simeq 10^3$ K and $Z\simlt 0.1
Z_\odot$, and even higher at higher metallicity, contrary to isobaric cooling
where it at least an order of magnitude lower. Despite this increase in
ionization fraction the gas-phase formation rate of molecular hydrogen (via
H$^-$) lowers with metallicity, because higher metallicity shorttens the
evolution time. We implement our self-consistent cooling rates into the
multi-dimensional parallel code ZEUS-MP in order to simulate evolution of a
supernova remnant, and compare it with an analogous model with tabulated
cooling rates published in previous works. We find significant differences
between the two descriptions, which may appear, e.g., in mixing of the ejected
metals in the circumstellar medium.
