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The Genesis of Super Star Clusters as Self-Gravitating HII Regions

  • Jonathan C. Tan
  • Christopher F. McKee
Part of the Springer Proceedings in Physics book series (SPPHY, volume 88)

Abstract

We examine the effects of ionization, radiation pressure and main sequence winds from massive stars on self-gravitating, clumpy molecular clouds, thereby modeling the formation and pre-supernova feedback of massive star clusters. We find the process of “turbulent mass loading” is effective in confining HII regions. Extrapolating typical Galactic high-mass star forming regions to greater initial gas cloud masses and assuming steady star formation rates, we determine the timescales for cloud disruption. We find that a dense (n c ≃ 2 x 105 cm−3) cloud with initial mass M c ≃ 4 x 105 M is able to form ~ 2 x 105 M of stars ( 50% efficiency) before feedback disperses the gas after ~ 3 Myr. This mass and age are typical of young, optically visible super star clusters (SSCs). The high efficiency permits the creation of a bound stellar system.

Keywords

Star Formation Massive Star Star Cluster Star Formation Rate Initial Mass Function 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag Berlin Heidelberg 2001

Authors and Affiliations

  • Jonathan C. Tan
    • 1
  • Christopher F. McKee
    • 2
  1. 1.Dept. of AstronomyUC BerkeleyBerkeleyUSA
  2. 2.Depts. of Physics and of AstronomyUC BerkeleyBerkeleyUSA

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