  We integrate numerically axially symmetric stationary Einstein equations
describing self-gravitating disks around spinless black holes. The numerical
scheme is based on a method developed by Shibata, but contains important new
ingredients. We derive a new general-relativistic Keplerian rotation law for
self-gravitating disks around spinning black holes. Former results concerning
rotation around spin-less black holes emerge in the limit of a vanishing spin
parameter. These rotation curves might be used for the description of rotating
stars, after appropriate modification around the symmetry axis. They can be
applied to the description of compact torus--black hole configurations,
including active galactic nuclei or products of coalescences of two neutron
stars.
