  We present models of turbulent mixing at the boundaries between hot
(T~10^{6-7} K) and warm material (T~10^4 K) in the interstellar medium, using a
three-dimensional magnetohydrodynamical code, with radiative cooling. The
source of turbulence in our simulations is a Kelvin-Helmholtz instability,
produced by shear between the two media. We found, that because the growth rate
of the large scale modes in the instability is rather slow, it takes a
significant amount of time (~1 Myr) for turbulence to produce effective mixing.
We find that the total column densities of the highly ionized species (C IV, N
V, and O VI) per interface (assuming ionization equilibrium) are similar to
previous steady-state non-equilibrium ionization models, but grow slowly from
log N ~10^{11} to a few 10^{12} cm^{-2} as the interface evolves. However, the
column density ratios can differ significantly from previous estimates, with an
order of magnitude variation in N(C IV)/N(O VI) as the mixing develops.
