  Observations of some starburst-driven galactic superwinds suggest that strong
radiative cooling could play a key role in the nature of feedback and the
formation of stars and molecular gas in star-forming galaxies. These
catastrophically cooling superwinds are not adequately described by adiabatic
fluid models, but they can be reproduced by incorporating non-equilibrium
radiative cooling functions into the fluid model. In this work, we have
employed the atomic and cooling module MAIHEM implemented in the framework of
the FLASH hydrodynamics code to simulate the formation of radiatively cooling
superwinds as well as their corresponding non-equilibrium ionization (NEI)
states for various outflow parameters, gas metallicities, and ambient
densities. We employ the photoionization program CLOUDY to predict radiation-
and density-bounded photoionization for these radiatively cooling superwinds,
and we predict UV and optical line emission. Our non-equilibrium
photoionization models built with the NEI states demonstrate the enhancement of
C IV, especially in metal-rich, catastrophically cooling outflows, and O VI in
metal-poor ones.
