H I and X-ray Emission in Simulations of the Interstellar Medium of Disk Galaxies

Details H I and X-ray Emission in Simulations of the Interstellar Medium of Disk Galaxies H I and X-ray Emission in Simulations of the Interstellar Medium of Disk Galaxies

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...184.2916r&link_type=abstract

American Astronomical Society, 184th AAS Meeting, #29.16; Bulletin of the American Astronomical Society, Vol. 26, p.904

Astronomy and Astrophysics

Astronomy

Scientific paper

Previously, we have generated six hydrodynamical two-dimensional two-fluid simulations of the interstellar medium that naturally create the filamentary structure of cold gas apparent in neutral hydrogen in the Galaxy. The two fluids in these simulations represent the stars and gas in the interstellar medium, and interact via star formation, mass loss, and heating from stellar winds or supernovae. The six simulations have different forms of the energy injection, by stellar winds or supernovae and stellar winds, and have three different rates. We analyze nine images from the simulations for the variation of H I column density with galactic latitude from three positions within bubbles of hot gas. In addition, we calculate the X-ray flux as well as the integrated X-ray flux at a number of distances from the same positions. We compare these with slices in latitude from H I and X-ray all-sky surveys, and show the relative contribution to the XRB of a local bubble. With the inclusion of X-ray absorption by cold and warm gas, we are able to calculate the frequency for and typical absorption of shadowing events.

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