Turbulent dissipation in the interstellar medium: implications for galaxy formation and evolution
We study turbulent dissipation in the ISM and explore some implications forgalaxy formation and evolution using 2D MHD numerical simulations of compress-ible uids. The turbulent kinetic energy Ek is injected by stellar sources formedself-consistently in the simulation. In the ISM-like uid, regimes o...
| Autores: | , |
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| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2000 |
| País: | México |
| Recursos: | Universidad Nacional Autónoma de México |
| Repositório: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57100913 |
| Acesso em linha: | https://www.redalyc.org/articulo.oa?id=57100913 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Física, Astronomía y Matemáticas In the ISM like uid ible uids Ek(t) decays (1+t) consistently in the simulation |
| Resumo: | We study turbulent dissipation in the ISM and explore some implications forgalaxy formation and evolution using 2D MHD numerical simulations of compress-ible uids. The turbulent kinetic energy Ek is injected by stellar sources formedself-consistently in the simulation. In the ISM-like uid, regimes of both forced anddecaying turbulence coexist. In the active turbulent regions (forced regime), Ek isdissipated locally and eciently. In the decaying regime (far from input sources),Ek(t) decays (1+t) |
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