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TURBULENT DISSIPATION IN THE INTERSTELLAR MEDIUM: IMPLICATIONS FOR GALAXY FORMATION AND EVOLUTION

We study turbulent dissipation in the ISM and explore some implications for galaxy formation and evolution using 2D MHD numerical simulations of compressible uids. The turbulent kinetic energy Ek is injected by stellar sources formed self-consistently in the simulation. In the ISM-like uid, regimes of both forced and decaying turbulence coexist. In the active turbulent regions (forced regime), Ek is dissipated locally and ecien tly. In the decaying regime (far from input sources), Ek(t) decays (1+t) 0:8 . The residual turbulent motions may propagate distances of the order of the disk height, suggesting that turbulence may be responsible for vertical support and star formation self-regulation at the disk level, but not at the level of the whole cosmological halo, as would be required in some models of galaxy formation.