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J/ApJ/689/919 Dynamical evolution of globular clusters (Prieto+, 2008)
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Beginning of ReadMe :J/ApJ/689/919 Dynamical evolution of globular clusters (Prieto+, 2008)
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Dynamical evolution of globular clusters in hierarchical cosmology.
Prieto J.L., Gnedin O.Y.
<Astrophys. J., 689, 919-935 (2008)>
=2008ApJ...689..919P (SIMBAD/NED BibCode)
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ADC_Keywords: Models, evolutionary ; Clusters, globular
Keywords: galaxies: formation - galaxies: kinematics and dynamics -
galaxies: star clusters - globular clusters: general
Abstract:
We test the hypothesis that metal-poor globular clusters form within
disk galaxies at redshifts z>3. We calculate the orbits of model
clusters in the time-variable gravitational potential of a Milky
Way-sized galaxy, using the outputs of a cosmological N-body
simulation. We find that at present the orbits are isotropic in the
inner 50kpc of the Galaxy and preferentially radial at larger
distances. All clusters located outside 10kpc from the center formed
in satellite galaxies, some of which are now tidally disrupted and
some of which survive as dwarf galaxies. Mergers of the progenitors
lead to a spheroidal spatial distribution of model clusters, although
it is more extended than that of Galactic metal-poor clusters and has
a somewhat shallower power-law slope of the number density profile,
gamma 2.7. The combination of two-body relaxation, tidal shocks, and
stellar evolution drives the evolution of the cluster mass function
from an initial power law to a peaked distribution, in agreement with
observations. However, not all initial conditions and not all
evolution scenarios are consistent with the observed mass function of
the Galactic globular clusters. We find that our best-fitting models
require the average cluster density, M/R^3^_h_, to be constant
initially for clusters of all mass and to remain constant with time.
However, these models do not explain the observed decrease of the mean
density with galactocentric distance. Both synchronous formation of
all clusters at a single epoch (z=4) and continuous formation over a
span of 1.6Gyr (between z=9 and 3) are consistent with the data. For
both formation scenarios, we provide online catalogs of the main
physical properties of model clusters.