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2012MNRAS.427.1940P - Mon. Not. R. Astron. Soc., 427, 1940-1952 (2012/December-2)
The mass function and dynamical mass of young star clusters: why their initial crossing-time matters crucially.
PARMENTIER G. and BAUMGARDT H.
Abstract (from CDS):
On the scale of individual clusters, we model the evolution of the ratio of the dynamical mass to luminous mass of a cluster after gas expulsion. Specifically, we map the radial dependence of the time-scale for a star cluster to return to equilibrium. We stress that fields of view a few pc in size only, typical of compact clusters with rapid evolutionary rates, are likely to reveal cluster regions which have returned to equilibrium even if the cluster experienced a major gas expulsion episode a few Myr earlier. We provide models with the aperture and time expressed in units of the initial half-mass radius and initial crossing-time, respectively, so that our results can be applied to clusters with initial densities, sizes, and apertures different from ours.
Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Journal keyword(s): stars: formation - stars: kinematics and dynamics - ISM: clouds - galaxies: star clusters: general
Simbad objects: 7
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