  The statistical properties of interstellar turbulence are studied by means of
three-dimensional high-resolution HD and MHD simulations of a SN-driven ISM. It
is found that the longitudinal and transverse turbulent length scales have time
averaged (over a period of 50 Myr) ratios of 0.5-0.6, almost similar to the one
expected for isotropic homogeneous turbulence. The mean characteristic size of
the larger eddies is found to be ~75 pc. Furthermore, the scalings of the
structure functions measured in the simulated disk show unambiguous departure
from the Kolmogorv (1941) model being consistent with the latest intermittency
studies of supersonic turbulence (Politano & Pouquet 1995; Boldyrev 2002). Our
results are independent of the resolution, indicating that convergence has been
reached, and that the unresolved smaller dissipative scales do not feed back on
the larger ones.
