Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.9707r&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #97.07; Bulletin of the American Astronomical Society, Vol. 24, p.1273
Other
Scientific paper
We have completed 2D hydrodynamical simulations in order to investigate the structure and kinematics of the interstellar medium. These simulations have been performed with a version of Zeus, an Eulerian finite-difference code, that has been modified to allow for two cospatial interacting fluids. One fluid represents the gas while the other represents a collection of mean Pop I stars. Star formation, stellar mass loss, and stellar wind heating couple the stars with the gas; radiative cooling in the gas is also included. In these simulations, one dimension is perpendicular to the plane (+/- 15 kpc) and the other is along the plane (2 kpc). Both the external gravitational potential and column density of gas used are appropriate for the Galaxy at the solar circle. The simulations generate a network of dense filaments of H I, which dominate the mass, extend up to 4--5 kpc above the midplane and surround large bubbles of warm and hot gas. These bubbles can reach sizes of up to many kpc's and are elongated perpendicular to the midplane. Dilute, hot (log T > 5.0) gas takes up most of the volume close to the midplane, with ~ 10% of the volume in each of the cold and warm gas phases. Also, we calculate scale heights of the three gas phases and the stars, velocity distributions of the cold gas, and compare these with observations. We wish to acknowedge the support of NASA Grant NAGW-2135.
Bregman Joel N.
Norman Michael L.
Rosen Alexander
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