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Nuclear Clusters in Dwarf Irregular Galaxies and Galactic GCs with Hot Horizontal Branches
A more
massive cluster will have a higher capability to retain stellar ejecta
than a lower mass one. This subsequently would lead to a higher degree
of self-enrichment with processed stellar ejecta from fast
evolving massive
stars. The degree of such self-enrichment should depend on the cluster
escape
velocity of stellar ejecta to reach its tidal radius and its
metallicity. Thus our primary goal
is to quantify and test the viability of such scenario by looking at
the escape velocity at the cluster tidal radius. We use the following
expression to calculate υesc:
where
rh and Mcl are the
cluster half-light radius in
parsecs and cluster
mass in M⊙; fc is a
coefficient which takes into account the dependence
of the escape velocity on the density profile of the cluster, i.e. its
concentration.
!Click
on image for full resolution!
Escape velocities for Nuclear clusters and Galactic EHB-GCs !Click on image for full resolution! To appear in Georgiev et al. in prep.
"A small nearby factory for massive star clusters"
!Click on image for full resolution!
Georgiev et
al. (2009b)
!Click
on image for full
resolution!
Da Rocha, Mieske, Georgiev, et al. (2010)
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