Statistics – Computation
Scientific paper
Apr 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..270..385w&link_type=abstract
Computational Star Formation, Proceedings of the International Astronomical Union, IAU Symposium, Volume 270, p. 385-388
Statistics
Computation
Ism: Clouds, Open Clusters And Associations: General, Galaxies: Star Clusters: General, Galaxies: Star Formation
Scientific paper
Super-star clusters are probably the largest star-forming entities in our local Universe, containing hundreds of thousands to millions of young stars usually within less than a few parsecs. While no such systems are known in the Milky Way (MW), they are found especially in pairs of interacting galaxies but also in some dwarf galaxies like R 136 in the Large Magelanic Cloud (LMC). With the use of SPH calculations we show that a natural explanation for this phenomenon is the presence of shear in normal spiral galaxies which facilitates the formation of low-density loose OB associations from giant molecular clouds (GMC) instead of dense super-star clusters. In contrast, in interacting galaxies and in dwarf galaxies, regions can collapse without having a large-scale sense of rotation. This lack of rotational support allows the giant molecular clouds to concentrate into a single, dense and gravitationally bound system.
Bonnell Ian A.
Weidner Carsten
Zinnecker Hans
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