Mixing Layer Theory and a Numerical Search for High Ions

Details Mixing Layer Theory and a Numerical Search for High Ions Mixing Layer Theory and a Numerical Search for High Ions

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...20311001l&link_type=abstract

American Astronomical Society Meeting 203, #110.01; Bulletin of the American Astronomical Society, Vol. 35, p.1378

Astronomy and Astrophysics

Astronomy

Scientific paper

Turbulent mixing layers have important implications for gas temperatures along ISM phase interfaces. Currently, however, mixing layer theory is based on many questionable assumptions and approximations, which may limit its accuracy. Here, we developed comprehensive MHD code to simulate the dynamics and cooling of mixing layers with high precision. Our code is fully three dimensional, includes non-equilibrium cooling, is capable of tracing heavy elements, contains realistic turbulence and will be high resolution. We hope to eventually use our results to explain observations of odd spectral data, primarily, the large excess in high ion absorption (e.g. OVI, NV, CIV). According to cooling theory, high ions are expected to cool and disappear very quickly, and therefore be rare components of the ISM. Our preliminary results show that mixing layers may be efficient enough to maintain intermediate zone gas temperatures and, therefore, maintain levels of high ion abundance in agreement with observed data.
This work was supported by a NSF-REU site grant (AST-0139563) to the University of Wisconsin-Madison.

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