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Turbulent dissipation in the interstellar medium: implications for galaxy formation and evolution | | V. Avila-Reese
; E. Vázquez-Semadeni
; | | Date: |
3 Dec 1999 | | Journal: | RevMexAA (Serie de Conferencias), vol. 9, p.63 | | Subject: | astro-ph | | Affiliation: | Instituto de Astronomia, UNAM, Mexico | | 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. | | Source: | arXiv, astro-ph/9912062 | | Services: | Forum | Review | PDF | Favorites | |
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