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We study, by means of adaptive mesh refinement hydro- andmagnetohydrodynamical simulations that cover a wide range of scales (from kpcto sub-parsec), the dimension of the most dissipative structures and theinjection scale of the turbulent interstellar gas, which we find to be about 75pc, in agreement with observations. This is however smaller than the averagesize of superbubbles, but consistent with significant density and pressurechanges in the ISM, which leads to the break-up of bubbles locally and hence toinjection of turbulence. The scalings of the structure functions are consistentwith log-Poisson statistics of supersonic turbulence where energy is dissipatedmainly through shocks. Our simulations are different from previous ones byother authors as (i) we do not assume an isothermal gas, but have temperaturevariations of several orders of magnitude and (ii) we have no artificialforcing of the fluid with some ad hoc Fourier spectrum, but drive turbulence bystellar explosions at the Galactic rate, self-regulated by density andtemperature thresholds imposed on the ISM gas.

The Generation and Dissipation of Interstellar Turbulence - Results from Large Scale High Resolution Simulations