Abstract
We summarize some observational comparison concerning the features of globular clusters (GCs) population in connection to the evolution of King models. We also make a comparison with some extragalactic GCs systems, in order to underline the effects of the main body on the dynamical evolution.
Highlights
Globular clusters (GCs), for their proprieties of symmetry and their high relaxation times, are important to test theories about thermodynamical stability of spherical self gravitating systems
The Harris catalogue includes Post-Core Collapse (PCC) globular clusters (GCs), namely GCs with collapsed cores that cannot be described by classical single mass King models profiles
We should expect that the peak value coincides with the known stability critical value W0 = 7.4, due to the old age of Milky Way (MW) GCs and the onset of the instability in the high W0 region
Summary
Globular clusters (GCs), for their proprieties of symmetry and their high relaxation times, are important to test theories about thermodynamical stability of spherical self gravitating systems. The last version (2010) of Harris GCs Catalogue (see Harris, 1996) includes 157 objects. Bica et al (2006) showed that the actual GCs population seems to have been contaminated by capture of smaller galaxies (and their possible GCs populations) during the Milky Way formation. Possible evidences of extragalactic origin of some GCs are retrograde motion (compared to galactic disk motion) and unusual young absolute age. It seems that the original GCs population suffered deep and incisive processes of disruption (see Aguilar et al, 1988; Hut & Djorgovski, 1992; Gnedin & Ostriker, 1997; Mackey & Gilmore, 2004), until almost 50% of original GCs are destroyed in the last Hubble time
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