MHD turbulent mixing layers
- Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St. Madison WI, 53706-1582 (United States)
- Department of Physics, University of Wisconsin-Whitewater, 800 W. Main Street, Whitewater, WI, 53190 (United States)
- Department of Physics, Wesleyan University, Middletown, CT 06459 (United States)
Turbulent mixing layers have been proposed to explain observations of line ratios of highly ionized elements in the interstellar medium. We present preliminary results of numerical simulations of turbulent mixing layers in a magnetized medium. We developed a MHD code with radiative cooling. The magnetic field is expected to be a controlling factor by suppressing instabilities that lead to the turbulent mixing. Our results suggest that the difference in turbulent mixing in the unmagnetized case as compared to the case of a weak magnetic field, {beta} = Pgas/Pmag {approx} 10, is insignificant. With a more thorough exploration of parameter space, this work will provide more reliable diagnostics of turbulent mixing layers than those available today.
- OSTI ID:
- 20719376
- Journal Information:
- AIP Conference Proceedings, Vol. 784, Issue 1; Conference: International conference on magnetic fields in the universe: From laboratory and stars to primordial structures, Angra dos Reis (Brazil), 28 Nov - 3 Dec 2004; Other Information: DOI: 10.1063/1.2077210; (c) 2005 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
- Country of Publication:
- United States
- Language:
- English
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