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K. Wada (National Astronomical Observatory, Japan)
Global structure and evolution of the multi-phase ISM are discussed, based on our high-resolution, two-dimensional hydrodynamical simulations of a self-gravitating gas disk in a galaxy. Energy feedback processes from the stellar wind and supernovae to the ISM are implemented with a few pc resolution in the few kpc-scale gas disk around a galactic center. Using our numerical code, we can study evolution of supernova remnants in a highly inhomogenous, multi-phase ISM, which has local turbulent-like motion as well as a global rotation. We find that low density, high temperature holes surrounded by high density, low temperature filaments/clumps are formed as a natural consequence of the non-linear evolution of the gas disk. This bubbly structure looks similar to the observed shell/hole structure of the ISM, but one should note that most hole-like structures in our simulations are not due to SNe. Statistical comparisons between models and observations, and effects of the Hubble sequence on the ISM will be discussed.
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