Formation of Compact Stellar Clusters by High-Redshift Galaxy Outflows
  II: Effect of Turbulence and Metal-Line Cooling
  In the primordial universe, low mass structures with virial temperatures less
than 10$^{4}$ K were unable to cool by atomic line transitions, leading to a
strong suppression of star formation. On the other hand, these "minihalos" were
highly prone to triggered star formation by interactions from nearby galaxy
outflows. In Gray & Scannapieco (2010), we explored the impact of
nonequilibrium chemistry on these interactions. Here we turn our attention to
the role of metals, carrying out a series of high-resolution three-dimensional
adaptive mesh refinement simulations that include both metal cooling and a
subgrid turbulent mixing model. Despite the presence of an additional coolant,
we again we find that outflow-minihalo interactions produce a distribution of
dense, massive stellar clusters. We also find that these clusters are evenly
enriched with metals to a final abundance of Z $\approx$ 10$^{-2}$ Z$_{\odot}$.
As in our previous simulations, all of these properties suggest that these
interactions may have given rise to present-day halo globular clusters.
