Fokker-Planck rotating models of globular clusters with black hole

We use 2D Fokker Planck axisymmetric rotating models of self-gravitating stellar systems (young clusters, globular clusters) with an embedded central massive/intermediate black hole. Our results confirme the acceleration of core collapse in single-mass rotating systems with black hole, with respect to the non-rotating case. At collapse time, the BH-potential (-GM_bh/r) dominates the stellar distribution in the core. The density distribution evolves to a power-law of λ = -1.75, according to n α r ^λ (Bahcall & Wolf 1976, Lightman & Shapiro 1977, Marchant & Shapiro 1980). Post-collapse evolution is driven through energy input from the central object. At this time the BH-mass is around 10 % of the initial cluster mass (M_cl) and the mass growth-rate reaches its maximum. The rotational velocity grows towards the center, inside the black hole influence radius, and the initial maximum at around the half-mass radius disappears slowly. After the collapse, the maximum of rotational speed (V _rot^max) at the center dominates. At later evolution times, up to the collapse and later, the system shows deviations from the King distribution f(E, J_z). Negative anisotropy (more circular than radial orbits) is observed in the central part as a consequence of the BH potential singularity (stellar radial orbits are accreted by the black hole). Our models can reproduce 2D distributions (in the meridional plane) of kinematical and structural parameters (density, dispersions, rotational velocity), covering a wide range of rotation rates, initial concentrations and ellipticities, which is aimed to enable observers to use them for comparisons with their data.