Simulations of radiative turbulent mixing layers
  Radiative turbulent mixing layers should be ubiquitous in multi-phase gas
with shear flow. They are a potentially attractive explanation for the high
ions such as OVI seen in high velocity clouds and the circumgalactic medium
(CGM) of galaxies. We perform 3D MHD simulations with non-equilibrium (NEI) and
photoionization modeling, with an eye towards testing simple analytic models.
Even purely hydrodynamic collisional ionization equilibrium (CIE) calculations
have column densities much lower than observations. Characteristic inflow and
turbulent velocities are much less than the shear velocity, and the layer width
$h \propto t_\mathrm{cool}^{1/2}$ rather than $h \propto t_\mathrm{cool}$.
Column densities are not independent of density or metallicity as analytic
scalings predict, and show surprisingly weak dependence on shear velocity and
density contrast. Radiative cooling, rather than Kelvin-Helmholtz instability,
appears paramount in determining the saturated state. Low pressure due to fast
cooling both seeds turbulence and sets the entrainment rate of hot gas, whose
enthalpy flux, along with turbulent dissipation, energizes the layer.
Regardless of initial geometry, magnetic fields are amplified and stabilize the
mixing layer via magnetic tension, producing almost laminar flow and depressing
column densities. NEI effects can boost column densities by factors of a few.
Suppression of cooling by NEI or photoionization can in principle also increase
OVI column densities, but in practice is unimportant for CGM conditions. To
explain observations, sightlines must pierce hundreds or thousands of mixing
layers, which may be plausible if the CGM exists as a `fog' of tiny cloudlets.
