The Turbulent Star Formation Model. Outline and Tests
| dc.creator | Vazquez-Semadeni, Enrique | |
| dc.date | 2003-09-26 | |
| dc.date.accessioned | 2026-07-07T02:09:47Z | |
| dc.date.available | 2026-07-07T02:09:47Z | |
| dc.description | We summarize the current status of the turbulent model of star formation in turbulent molecular clouds. In this model, clouds, clumps and cores form a hierarchy of nested density fluctuations caused by the turbulence, and either collapse or re-expand. Cores that collapse can be either internally sub- or super-sonic. The former cannot further fragment, and can possibly be associated with the formation of a single or a few stars. The latter, instead, can undergo turbulent fragmentation during their collapse, and probably give rise to a cluster of bound objects. The star formation efficiency is low because only a small fraction of the density fluctuations proceed to collapse. Those that do not may constitute a class of ``failed'' cores that can be associated with the observed starless cores. ``Synthetic'' observations of cores in numerical simulations of non-magnetic turbulence show that a large fraction of them have subsonic internal velocity dispersions, can be fitted by Bonnor-Ebert column density profiles, and exhibit ``coherence'' (an apparent independence of linewidth with column density near the projected core centers), in agreement with observed properties of molecular cloud cores. | |
| dc.description | 8 pages, 2 figures. To appear in the Proceedings of IAU Symposium 221, "Star Formation at High Angular Resolution", Editors M. Burton, R. Jayawardhana & T. Bourke, Astronomical Society of the Pacific | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0309717 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0309717 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/6566 | |
| dc.subject | Astrophysics | |
| dc.title | The Turbulent Star Formation Model. Outline and Tests | |
| dc.type | text |