Physics
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993egte.conf..322s&link_type=abstract
In NASA. Ames Research Center, The Evolution of Galaxies and Their Environment p 322-323 (SEE N93-26706 10-90)
Physics
Interstellar Matter, Seyfert Galaxies, Shear Flow, Space Plasmas, Stellar Winds, Supernovae, Turbulent Boundary Layer, Turbulent Mixing, Emission Spectra, Extreme Ultraviolet Radiation, High Reynolds Number, Infrared Radiation, Light Emission, Turbulence, Ultraviolet Emission, Viscosity
Scientific paper
We propose that turbulent mixing layers are common in the interstellar medium (ISM). Injection of kinetic energy into the ISM by supernovae and stellar winds, in combination with density and temperature inhomogeneities, results in shear flows. Such flows will become turbulent due to the high Reynolds number (low viscosity) of the ISM plasma. These turbulent boundary layers will be particularly interesting where the shear flow occurs at boundaries of hot (approximately 10(exp 6) K) and cold or warm (10(exp 2) - 10(exp 4) K) gas. Mixing will occur in such layers producing intermediate-temperature gas at T is approximately equal to 10(exp 5.0) - 10(exp 5.5) that radiates strongly in the optical, ultraviolet, and EUV. We have modeled these layers under the assumptions of rapid mixing down to the atomic level and steady flow. By including the effects of non-equilibrium ionization and self-photoionization of the gas as it cools after mixing, we predict the intensities of numerous optical, infrared, and ultraviolet emission lines, as well as absorption column densities of C 4, N 5, Si 4, and O 6.
Begelman Mitchell C.
Shull Michael J.
Slavin Jonathan D.
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