AAS Meeting #194 - Chicago, Illinois, May/June 1999
Session 64. Shells in the Global ISM
Topical, Oral, Wednesday, June 2, 1999, 8:30-10:00am, 10:45am-12:30pm, 2:00-3:30pm, Continental Ballroom B

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[64.07] Bubbly Structure in the Multi-Phase ISM without Star Formation

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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