Super Massive Star Clusters: From Superwinds to a Cooling Catastrophe and the Re-processing of the Injected Gas
arXiv:astro-ph/0610573 · doi:10.1017/S1743921307001548
Abstract
Different hydrodynamic regimes for the gaseous outflows generated by multiple supernovae explosions and stellar winds occurring within compact and massive star clusters are discussed. It is shown that there exists the threshold energy that separates clusters whose outflows evolve in the quasi-adiabatic or radiative regime from those within which catastrophic cooling and a positive feedback star-forming mode sets in. The role of the surrounding ISM and the observational appearance of the star cluster winds evolving in different hydrodynamic regimes are also discussed.
arXiv comment4 pages, 2 figures, to be published in the Proceedings IAU Symposium 237 "Triggered Star Formation in a Turbulent ISM", eds. B.G. Elmegreen & J. Palous
References in corpus (6)
- Kinematic Masses of Super Star Clusters in M82 from High-Resolution Near-Infrared Spectroscopy
- Winds driven by super-star clusters: The self-consistent radiative solution
- HST/STIS Spectroscopy of Five Super Star Clusters in the Starburst Galaxy M82
- The Cluster Wind from Local Massive Star Clusters
- On the X-ray Emission from Massive Star Clusters and their Evolving Superbubbles
- On the Extreme Positive Feedback Star-Forming Mode from Massive and Compact Superstar Clusters