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Time-dependent cooling processes are of paramount importance in the evolutionof astrophysical gaseous nebulae and, in particular, when radiative shocks arepresent. The present work introduces a necessary set of tools that can be usedto model radiative astrophysical flows in the optically-thin plasma limit. Weaim to provide reliable and accurate predictions of emission line ratios andradiative cooling losses in astrophysical simulations of shocked flows.Moreover, we discuss numerical implementation aspects to ease futureimprovements and implementation in other MHD numerical codes. The mostimportant source of radiative cooling for our plasma conditions comes from thecollisionally-excited line radiation. We evolve a chemical network, including29 ion species, to compute the ionization balance in non-equilibriumconditions. After a series of validations and tests, typical astrophysicalsetups are simulated in 1D and 2D, employing both the present cooling model anda simplified one. The influence of the cooling model on structure morphologiescan become important, especially for emission line diagnostic purposes.

Simulating radiative astrophysical flows with the PLUTO code: A non-equilibrium, multi-species cooling function