Self-enrichment in Omega Centauri
| dc.creator | Ikuta, C. | |
| dc.creator | Arimoto, N. | |
| dc.date | 1999-12-28 | |
| dc.date.accessioned | 2026-07-07T02:35:12Z | |
| dc.date.available | 2026-07-07T02:35:12Z | |
| dc.description | The origin of abundance spreads observed in omega Centauri is studied in the context of the self-enrichment scenario. Five chemical evolution models are constructed and are compared with empirical metallicity distribution of $ω$ Cen. After a series of simulations, it is found that neither of closed-box, outflow, nor infall models can reproduce the empirical metallicity distribution of omega Cen, while a modified outflow model with a bimodal initial mass function (IMF) gives a metallicity distribution that fits closely to the empirical ones. In the modified outflow model, long-lived stars are assumed to form after the first explosion of type II supernovae (SNII) in a proto-cloud. The modified outflow model involves gas infall at the very first chemical evolution. Thus we conclude that self-enrichment causes the abundance dispersion in omega Cen. A success of the outflow model with the bimodal IMF implies that low mass stars in a globular cluster (GC) should have formed in the gas already enriched by the first generation of SNII. This scenario, originally proposed by Cayrel (1986), can explain a lack of globular clusters with [Fe/H] > -2.2 in the Milky Way Galaxy. | |
| dc.description | 35 pages, 9 figures. Accepted for publication in A&A, Main Journal | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9912526 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9912526 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/15529 | |
| dc.subject | Astrophysics | |
| dc.title | Self-enrichment in Omega Centauri | |
| dc.type | text |