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The results of a three-dimensional model for disc-halo interaction are presented here. The model considers explicitly the input of energy and mass by isolated and correlated supernovae in the disc. Once disrupted by the explosions, the disc never returns to its initial state. Instead it approaches a state where a thin H i disc is formed in the Galactic plane, overlaid by thick H i and H ii gas discs with scaleheights of 500 pc and 1–1.5 kpc, respectively. The upper parts of the thick H ii disc (the diffuse ionized medium) act as a disc-halo interface, and its formation and stability are directly correlated to the supernova rate per unit area in the simulated disc.
Miguel A. de Avillez (Sat,) studied this question.