Dynamics of Black Hole Clusters with Rotation

Details Dynamics of Black Hole Clusters with Rotation Dynamics of Black Hole Clusters with Rotation

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002bhap.conf..249l&link_type=abstract

BLACK HOLE ASTROPHYSICS 2002 . Proceedings of the Sixth APCTP Winter School . Held 9-12 January 2002 in Pohang, Korea. Edited by

Astronomy and Astrophysics

Astrophysics

Scientific paper

The rapid evolution of high mass stars can form black holes in a short time scale (< 107 years). The stellar systems in galactic nuclei can be assumed to be composed of low mass stars and stellar mass black holes. The typical mass of such black holes is about 10 M&sun; which is much greater than the typical mass of ordinary stars that comprise most of the mass in the cluster. In such a situation, black holes quickly form a subsystem within the core of the cluster of ordinary stars. The subsystem evolves on its own relaxation time scale which is very short. The gravitational radiation can lead to the merger of binaries instead of being ejected from the cluster. A central seed black hole of mass comparable to the central core of the black hole subsystem could form if the stellar system has velocity dispersion greater than certain limit (which is estimated to be around 500 km/sec). The presence of the rotation of the cluster can further accelerate the dynamical evolution.

Affiliated with

Also associated with

No associations

Rating

Dynamics of Black Hole Clusters with Rotation does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Dynamics of Black Hole Clusters with Rotation, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Dynamics of Black Hole Clusters with Rotation will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1312634