Feature and evolution of globular clusters. (II). The formation and dynamical evolution of GC.

Details Feature and evolution of globular clusters. (II). The formation and dynamical evolution of GC. Feature and evolution of globular clusters. (II). The formation and dynamical evolution of GC.

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pabei...9...22m&link_type=abstract

Prog. Astron., Vol. 9, No. 1, p. 22 - 31

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Scientific paper

Various evolution time-scales for GC have been analysed. The two-body collisional process is quick enough for the GC relaxation within the Hubble time, but the violent relaxation is needed for bigger systems like E galaxies. Fully relaxed, GC will settle into a quasi-equilibrium state which can be described by the King model. But the evaporation and interaction with outer gravitational fields will cause the GC to evolve from one King state to another, until the gravo-thermal instability starts and the core collapses. Observation confirms the theoretical prediction of core collapse and finds 1/5 GC have collapsed. But there is no catastrophe, the binary formation will stop the core collapse and a power-law density profile will form. At the end, the process concerning the GC formation is briefly mentioned.

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