  We have developed a two-dimensional orbit averaged Fokker-Planck model of
stellar clusters which expands on spherically symmetric one-dimensional models
to include rotation and ellipticity. Physical effects such as collisions,
finite stellar lifetimes and bar formation (i.e., a non-axisymmetric component
of the potential) can also be included. The first use of the model is to study
the evolution of dense clusters (rho(r=0)=~10^7 M_sun/pc^3) that may be
expected to have existed at the centres of newly-forming galaxies, with the
goal of verifying that angular momentum can be removed from the core of the
cluster quickly enough so that rotation no longer prevents the formation of a
massive (~10^2 M_sun) object. This could act as the seed black hole for the
formation of an AGN.
