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- W2155646530 abstract "We study turbulent dissipation in the ISM and explore some implications for galaxy formation and evolution using 2D MHD numerical simulations of compressible fluids. The turbulent kinetic energy E_k is injected by stellar sources formed self-consistently in the simulation. In the ISM-like fluid, regimes of both forced and decaying turbulence coexist. In the active turbulent regions (forced regime), E_k is dissipated locally and efficiently. In the decaying regime (far from input sources), E_k(t) decays ~(1+t)^-0.8. The residual turbulent motions may propagate distances of the order of the observed disk height, suggesting that turbulence may be the responsible of 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." @default.
- W2155646530 created "2016-06-24" @default.
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- W2155646530 date "1999-12-03" @default.
- W2155646530 modified "2023-09-25" @default.
- W2155646530 title "Turbulent dissipation in the interstellar medium: implications for galaxy formation and evolution" @default.
- W2155646530 hasPublicationYear "1999" @default.
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