The Birth, Evolution and Death of Star Clusters
| dc.creator | Kroupa, Pavel | |
| dc.date | 2000-10-19 | |
| dc.date | 2000-10-20 | |
| dc.date.accessioned | 2026-07-07T01:56:07Z | |
| dc.date.available | 2026-07-07T01:56:07Z | |
| dc.description | A dense-enough gas-accumulation evolves, over a few Myr of intensifying star formation, to an embedded cluster. If it contains a sufficient amount of mass, O stars form and explosively expel the remaining gas, whereas poorer clusters reduce their embryonic gas content more gradually. The sudden expulsion of gas unbinds most of a rich cluster, but a significant fraction of it can condense by two-body interactions to become an open cluster despite a star-formation efficiency as low as 30 per cent. Poorer clusters survive their gradual mass loss more easily, but have short, relaxation-limited life-times. Pleiades-like clusters may thus form as nuclei of expanding OB associations, by filling their tidal radii and having large (1-2 pc) core-radii. A 'main-sequence' of clusters is thus established. Ultimately, a cluster dies an explosive death through the ever shortening relaxation time, and leaves a remnant that consists of about 4-10 stars arranged in a highly hierarchical and thus long-lived system. Dynamical mass segregation in very young clusters is extremely rapid, and heats a cluster substantially, which is partially off-set by the cooling from the disruption of primordial binaries. | |
| dc.description | Invited talk, to appear in Asp.Conf.Series, Origin and Evolution of Young Stellar Clusters, 12 pages, 3 figures, replaced version has completed references | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0010405 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0010405 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/1886 | |
| dc.subject | Astrophysics | |
| dc.title | The Birth, Evolution and Death of Star Clusters | |
| dc.type | text |