The dynamical evolution of dense star clusters in galactic nuclei

Details The dynamical evolution of dense star clusters in galactic nuclei The dynamical evolution of dense star clusters in galactic nuclei

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..483q&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 20, 1990, p. 483-500. Research supported by the U.S. Army.

Astronomy and Astrophysics

Astronomy

115

Galactic Nuclei, Star Clusters, Stellar Evolution, Stellar Motions, Binary Stars, Black Holes (Astronomy), Gravitational Effects, Star Formation, Stellar Mass

Scientific paper

The results of numerical Fokker-Planck calculations of the dynamical evolution of dense, spherical star clusters in galactic nuclei are presented. The clusters initially contain solar-mass, main-sequence stars at densities and velocity dispersions similar to those observed in dense but otherwise normal galactic nuclei. In clusters with initial relaxation time scales t(r) less than about 10 to the 8th yr, stars of mass greater than about 100 solar masses easily form through multiple stellar mergers at the cluster center. The massive stars form before there is a significant rise in the central velocity dispersion. These massive stars can undergo further mergers and collapse to form the seed black holes that have been assumed as initial data in simulations of active galactic nuclei and quasars. Stellar mergers followed by supernovae can lead to dense clusters of compact stellar remnants in galactic nuclei. These clusters are important sources of gravitational radiation.

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