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Session 111 - Massive Black Holes and Dynamics of Galaxy Cores.
Oral session, Thursday, January 16
Harbour A,
We present simulations of the evolution of dense star clusters integrated using a two-dimensional Fokker-Planck approach. Effects of initial rotation, ellipticity, and stellar mergers are included. When an instability criterion is satisfied (T_rot/|W| > \alpha, where \alpha is the stability parameter), a non-axisymmetric component of the potential is applied to model the formation of a stellar bar. Results are interpreted with a view to describing the formation of a massive (\sim10^3 M_ødot) object near the cluster center which could evolve into the seed black hole of an AGN or quasar.
The author(s) of this abstract have provided an email address for comments about the abstract: girash@skyron.harvard.edu