Formation of globular clusters in galaxy mergers
| dc.creator | Bekki, Kenji | |
| dc.creator | Couch, Warrick J. | |
| dc.creator | Forbes, Duncan A. | |
| dc.creator | Beasley, M. A. | |
| dc.date | 2003-08-15 | |
| dc.date.accessioned | 2026-07-07T02:09:14Z | |
| dc.date.available | 2026-07-07T02:09:14Z | |
| dc.description | Our numerical simulations first demonstrate that the pressure of ISM in a major merger becomes so high ($>$ $10^5$ $\rm k_{\rm B}$ K $\rm cm^{-3}$) that GMCs in the merger can collapse to form globular clusters (GCs) within a few Myr. The star formation efficiency within a GMC in galaxy mergers can rise up from a few percent to $\sim$ 80 percent, depending on the shapes and the temperature of the GMC. This implosive GC formation due to external high pressure of warm/hot ISM can be more efficient in the tidal tails or the central regions of mergers. The developed clusters have King-like profile with the effective radius of a few pc. The structural, kinematical, and chemical properties of these GC systems can depend on orbital and chemical properties of major mergers. | |
| dc.description | 2 pages 1 figure (color), in the proceedings of Extragalactic Globular clusters and their host galaxies (JD6 in IAU) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0308263 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0308263 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/6357 | |
| dc.subject | Astrophysics | |
| dc.title | Formation of globular clusters in galaxy mergers | |
| dc.type | text |