Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...517..829m&link_type=abstract
The Astrophysical Journal, Volume 517, Issue 2, pp. 829-840.
Astronomy and Astrophysics
Astronomy
2
Hydrodynamics, Ism: Clouds, Methods: N-Body Simulations, Galaxy: Open Clusters And Associations: General, Stars: Formation
Scientific paper
We report on the results of N-body simulations of star formation resulting from mergers during the collapse of dynamically cold, flattened systems of cloudlets. Such evolution is expected to occur in several models of cluster star formation. As was found previously in the case of spherical systems, the resulting star clusters have half-mass radii that are significantly smaller than the initial values for the systems. Stars that form early in the collapse have large final orbital radii and retain a strong memory of the initial ellipticity of the system. Stars that form later have smaller final radii and retain less memory. If we examine only those stars within the final half-mass radii of the models, we find that they follow a much less ellipsoidal distribution than do stars at larger radii. Their ellipticities, however, generally exceed those of young, dynamically unevolved massive star clusters in the LMC. The best comparisons with the observed ellipticities are found in models for which the initial system minor-to-major axis ratios b/a>~0.2, system kinetic-to-potential energy ratios Q>~0.1, covering factors f_tau<~0.2, or initial cloud masses M_i<
Murray Stephen D.
Raymondson Daisy A.
Urbanski Rachel A.
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