Halo enrichment by disrupted globular clusters
| dc.creator | Baumgardt, H. | |
| dc.date | 2000-12-21 | |
| dc.date.accessioned | 2026-07-07T01:57:09Z | |
| dc.date.available | 2026-07-07T01:57:09Z | |
| dc.description | We study the evolution of the galactic globular cluster system to determine its initial mass-function and the fraction of halo stars that could have come from disrupted globular clusters. We study the cluster evolution under the influence of two destruction mechanisms: Two-body relaxation and dynamical friction. New results of N-body simulations are used for the lifetimes of clusters dissolving under the influence of two-body relaxation. Two different mass-functions are studied: A gaussian initial distribution in log(M_C) with mean mass and scatter similar to what one observes for the galactic globular cluster system, and a power-law distribution resembling what is seen for clusters in merging and interacting galaxies. We find that in the inner parts of the galaxy, both distributions evolve in such a way that they are consistent with the observations. In the outer parts, a gaussian initial distribution gives the better fit. This might change however if elliptic orbits are considered, or there are undiscovered low-mass clusters in the galactic halo. In any case, only a small fraction of the stellar halo of the Milky Way originated in globular clusters. | |
| dc.description | 7 pages, 3 figures, to appear in 'Modes of Star Formation', eds. Eva Grebel & Wolfgang Brandner, ASP Conf. Ser | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0012468 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0012468 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2272 | |
| dc.subject | Astrophysics | |
| dc.title | Halo enrichment by disrupted globular clusters | |
| dc.type | text |