An MHD Study of Turbulent Mixing Layers

Details An MHD Study of Turbulent Mixing Layers An MHD Study of Turbulent Mixing Layers

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.3813e&link_type=abstract

American Astronomical Society Meeting 206, #38.13; Bulletin of the American Astronomical Society, Vol. 37, p.492

Astronomy and Astrophysics

Astronomy

Scientific paper

Observations of highly ionized species (O VI, C IV, N V, Si IV ) in the interstellar medium (ISM) indicate the existence of substantial amounts of plasma at Temperatures of T ˜ 105. To explain the line ratios observed, it has been proposed to be the result of mixing by turbulence at the interfaces between hot (T ˜ 106) and warm (T ˜ 104) media. In addition, the the ISM is magnetized. And the magnetic field is expected to be a controlling factor that can suppress the instabilities that lead to the onset of turbulence at such interfaces. We present results of numerical simulations of turbulent mixing layers, using a MHD code with radiative cooling. With a more complete exploration of parameter space, this work will provide more reliable diagnostics of turbulent mixing layers than those available today.

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