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Super massive star clusters: from superwinds to a cooling catastrophe and the re-processing of the injected gas

Published online by Cambridge University Press:  01 August 2006

S. Silich ,
G. Tenorio-Tagle ,
C. Muñoz-Tuñón  and
J. Palouš
S. Silich
Affiliation:
Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla, México email: silich@inaoep.mx
G. Tenorio-Tagle
Affiliation:
Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla, México email: silich@inaoep.mx
C. Muñoz-Tuñón
Affiliation:
Instituto de Astrofísica de Canarias, E 38200 La Laguna, Tenerife, Spaincmt@ll.iac.es
J. Palouš
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II 1401, 141 31 Prague, Czech Republic email: palous@ig.cas.cz
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Abstract

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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.

Keywords

galaxies: star clustersgalaxies: starburstISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 242 - 245
Copyright
Copyright © International Astronomical Union 2007

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