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The ISM, powered by SNe, is turbulent and permeated by a magnetic field (witha mean and a turbulent component). It constitutes a frothy medium that ismostly out of equilibrium and is ram pressure dominated on most of thetemperature ranges, except for T< 200 K and T> 1E6 K, where magnetic andthermal pressures dominate, respectively. Such lack of equilibrium is alsoimposed by the feedback of the radiative processes into the ISM flow. Manymodels of the ISM or isolated phenomena, such as bubbles, superbubbles, cloudsevolution, etc., take for granted that the flow is in the so-called collisionalionization equilibrium (CIE). However, recombination time scales of most of theions below 1E6 K are longer than the cooling time scale. This implies that therecombination lags behind and the plasma is overionized while it cools. As aconsequence cooling deviates from CIE. This has severe implications on theevolution of the ISM flow and its ionization structure. Here, besides reviewingseveral models of the ISM, including bubbles and superbubbles, the validity ofthe CIE approximation is discussed, and a presentation of recent developmentsin modeling the ISM by taking into account the time-dependent ionizationstructure of the flow in a full-blown numerical 3D high resolution simulationis presented.

The Evolution of the Large-scale ISM: Bubbles, Superbubbles and Non-Equilibrium Ionization