Atomic Chemistry in Turbulent Astrophysical Media II: Effect of the
  Redshift Zero Metagalactic Background
  We carry out direct numerical simulations of turbulent astrophysical media
exposed to the redshift zero metagalactic background. The simulations assume
solar composition and explicitly track ionizations, recombinations, and
ion-by-ion radiative cooling for hydrogen, helium, carbon, nitrogen, oxygen,
neon, sodium, magnesium, silicon, sulfur, calcium, and iron. Each run reaches a
global steady state that not only depends on the ionization parameter, $U,$ and
mass-weighted average temperature, $T_{\rm MW},$ but also on the the
one-dimensional turbulent velocity dispersion, \soned. We carry out runs that
span a grid of models with $U$ ranging from 0 to 10$^{-1}$ and \soned\ ranging
from 3.5 to 58 km s$^{-1}$, and we vary the product of the mean density and the
driving scale of the turbulence, $nL,$ which determines the average temperature
of the medium, from $nL =10^{16}$ to $nL =10^{20}$ cm$^{-2}$. The turbulent
Mach numbers of our simulations vary from $M \approx 0.5$ for the lowest
velocity dispersions cases to $M \approx 20$ for the largest velocity
dispersion cases. When $M \lesssim1,$ turbulent effects are minimal, and the
species abundances are reasonably described as those of a uniform photoionized
medium at a fixed temperature. On the other hand, when $M \gtrsim 1,$ dynamical
simulations such as the ones carried out here are required to accurately
predict the species abundances. We gather our results into a set of tables, to
allow future redshift zero studies of the intergalactic medium to account for
turbulent effects.
