Turbulent dissipation in the interstellar medium: implications for galaxy formation and evolution
| dc.creator | Avila-Reese, V. | |
| dc.creator | Vázquez-Semadeni, E. | |
| dc.date | 1999-12-03 | |
| dc.date | 2000-04-26 | |
| dc.date.accessioned | 2026-07-25T21:22:50Z | |
| dc.description | 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. | |
| dc.description | 3 pages, uses rmaa.cls, to appear in "Astrophysical Plasmas: Codes, Models, and Observations", Eds. J. Franco, J. Arthur, N. Brickhouse, Rev.Mex.AA Conf. Series. An error in the calculation of the dissipation time, t_d, was corrected (it referred to the dissipation in the forced regions). Now we report the global t_d, which is the relevant quantity for the whole flow | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9912062 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9912062 | |
| dc.identifier | RevMexAA (Serie de Conferencias), vol. 9, p.63 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/78933 | |
| dc.subject | Astrophysics | |
| dc.title | Turbulent dissipation in the interstellar medium: implications for galaxy formation and evolution | |
| dc.type | text |