Astronomy and Astrophysics – Astrophysics
Scientific paper
1999-12-03
RevMexAA (Serie de Conferencias), vol. 9, p.63
Astronomy and Astrophysics
Astrophysics
3 pages, uses rmaa.cls, to appear in "Astrophysical Plasmas: Codes, Models, and Observations", Eds. J. Franco, J. Arthur, N. B
Scientific paper
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.
Avila-Reese Vladimir
Vázquez-Semadeni Enrique
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