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Turbulent mixing layers in the interstellar medium of galaxiesWe 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.
Document ID
19930017674
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Slavin, J. D. (Colorado Univ. Boulder, CO, United States)
Shull, J. M. (Colorado Univ. Boulder, CO, United States)
Begelman, M. C. (Colorado Univ. Boulder, CO, United States)
Date Acquired
September 6, 2013
Publication Date
January 1, 1993
Publication Information
Publication: NASA. Ames Research Center, The Evolution of Galaxies and Their Environment
Subject Category
Astrophysics
Accession Number
93N26863
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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IDRelationTitle19930017517Collected WorksThe Evolution of Galaxies and Their Environment
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