High-Resolution Modelling of the Disk-Halo Interaction

Astronomy and Astrophysics – Astrophysics

Scientific paper

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Scientific paper

Large scale modelling of the interstellar gas in the disk and halo has been carried out with a three-dimensional code that uses adaptive mesh refinement (AMR). The model includes a gravitational field provided by the stars in the disk, an ideal-gas equation of state, and an approximation for the cooling curve, assuming collisional ionization equilibrium. Supernovae are set up both isolated and in associations, in a manner compatible with observations. Once disrupted by the explosions, the disk never returns to its initial state, regardless of the initial vertical distribution of the disk gas, provided enough supernovae occur. Instead a thin HI disk forms in the Galactic plane, and, above and below, a thick inhomogeneous gas disk forms, with scale heights in HI of 500 pc and in HII of 1 kpc. The upper parts of the thick HII disk form the disk-halo interface, where a large scale fountain is set up by hot ionized gas escaping in a turbulent convective flow.

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