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arXiv:astro-ph/0012005 (astro-ph)
[Submitted on 1 Dec 2000]

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

Authors:Jonathan C. Tan (1), Christopher F. McKee (1,2) ((1) Dept. of Astronomy, UC Berkeley; (2) Dept. of Physics, UC Berkeley)
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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 10^5 cm^-3 cloud with initial mass M_c ~ 4 x 10^5 M_sun is able to form ~2 x 10^5 M_sun 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.
Comments: To appear in Proceedings of "Starbursts: Near and Far", Ringberg Castle, Germany, 10-15 September 2000; 6 pages (including 1 figure)
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/0012005
  (or arXiv:astro-ph/0012005v1 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/0012005

Submission history

From: Jonathan C. Tan [view email]
[v1] Fri, 1 Dec 2000 01:13:28 UTC (30 KB)
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