Physics
Scientific paper
Jun 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.405..194f&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 1, pp. 194-208.
Physics
4
Black Hole Physics, Gravitation, Stellar Dynamics, Methods: Numerical, Globular Clusters: General, Galaxies: Nuclei
Scientific paper
The evolution of self-gravitating rotating dense stellar systems (e.g. globular clusters, galactic nuclei) with embedded black holes is investigated. The interaction between the black hole and the stellar component in differentially rotating flattened systems is analysed. The interplay between velocity diffusion resulting from relaxation and black hole star accretion is investigated, together with cluster rotation, using 2D+1 (20 in space and time) Fokker-Planck numerical methods. The models can reproduce the Bahcall-Wolf solution f ~ E1/4 (n ~ r-7/4) inside the zone of influence of the black hole. Gravo-gyro and gravo-thermal instabilities cause the system to have a faster evolution, leading to shorter collapse times with respect to non-rotating systems. Angular momentum transport and star accretion support the development of central rotation on relaxation time-scales. We explore system dissolution as a result of mass loss in the presence of an external tidal field (e.g. for globular clusters in galaxies).
Fiestas Jose
Spurzem Rainer
No associations
LandOfFree
Dynamical evolution of rotating dense stellar systems with embedded black holes 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 Dynamical evolution of rotating dense stellar systems with embedded black holes, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Dynamical evolution of rotating dense stellar systems with embedded black holes will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1579437