Global Star Formation in the Multi-Phase ISM

Details Global Star Formation in the Multi-Phase ISM Global Star Formation in the Multi-Phase ISM

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...36w&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

1

Scientific paper

Using high resolution, two-dimensional hydrodynamical simulations, we investigate the evolution of a self-gravitating multi-phase interstellar medium in a galaxy modeling the Large Magellanic Clouds (LMC). We compare the observations of HI and molecular gas with the numerically obtained HI and CO brightness temperature distribution. The morphology and statistical quantities of the numerical HI and CO maps are similar to the observed one. Our numerical model for the star formation allows us to follow the evolution of the blastwaves due to supernovae in the inhomogeneous, multi-phase, and turbulent-like media self-consistently. A model with energy feedback shows that kpc-scale low density holes or dense shells seen in the observed HI map are barely formed under frequent supernovae. Kpc-scale holes can be formed due to nonlinear evolution of the gravitational instability in the rotating disk.

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