The formation, disruption and properties of pressure-supported stellar systems and implications for the astrophysics of galaxies
arXiv:0712.2818 · doi:10.1017/S1743921308015202
Abstract
Most stars form in dense star clusters deeply embedded in residual gas. These objects must therefore be seen as the fundamental building blocks of galaxies. With this contribution some physical processes that act in the very early and also later dynamical evolution of dense stellar systems in terms of shaping their later appearance and properties, and the impact they have on their host galaxies, are highlighted. Considering dense systems with increasing mass, it turns out that near 10^6 Msol their properties change fundamentally: stellar populations become complex, a galaxial mass--radius relation emerges and the median two-body relaxation time becomes longer than a Hubble time. Intriguingly, only systems with a two-body relaxation time longer than a Hubble time show weak evidence for dark matter, whereby dSph galaxies form total outliers.
10 pages, to appear in IAUS246: Dynamical Evolution of Dense Stellar Systems, eds: E. Vesperini, M. Giersz, A. Sills
References in corpus (8)
- Slow Star Formation in Dense Gas: Evidence and Implications
- Gas expulsion and the destruction of massive young clusters
- Evidence for the Strong Effect of Gas Removal on the Internal Dynamics of Young Stellar Clusters
- Do O-stars form in isolation?
- The Origin of the Gaussian Initial Mass Function of Old Globular Cluster Systems
- On the infant weight loss of low- to intermediate-mass star clusters
- Captured older stars as the reason for apparently prolonged star formation in young star clusters
- Complex stellar populations in massive clusters: trapping stars of a dwarf-disc galaxy in a newborn stellar super-cluster