Formation of Young Star Clusters
| dc.creator | Elmegreen, Bruce G. | |
| dc.date | 2004-05-28 | |
| dc.date.accessioned | 2026-07-07T02:13:20Z | |
| dc.date.available | 2026-07-07T02:13:20Z | |
| dc.description | Turbulence, self-gravity, and cooling convert most of the interstellar medium into cloudy structures that form stars. Turbulence compresses the gas into clouds directly and it moves pre-existing clouds around passively when there are multiple phases of temperature. Self-gravity also partitions the gas into clouds, forming giant regular complexes in spiral arms and in resonance rings and contributing to the scale-free motions generated by turbulence. Dense clusters form in the most strongly self-gravitating cores of these clouds, often triggered by compression from local stars. Pre-star formation processes inside clusters are not well observed, but the high formation rates and high densities of pre-stellar objects, and their power law mass functions suggest that turbulence, self-gravity, and energy dissipation are involved there too. | |
| dc.description | 6 pages, In Dynamics and Evolution of Dense Stellar Systems, IAU Joint Discussion 11, Sydney Australia, July 18, 2004 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0405579 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0405579 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/7780 | |
| dc.subject | Astrophysics | |
| dc.title | Formation of Young Star Clusters | |
| dc.type | text |