  We discuss a clumpy model of obscuring dusty tori around AGN. Cloud-cloud
collisions lead to an effective viscosity and a geometrically thick accretion
disk, which has the required properties of a torus.
  Accretion in the combined gravitational potential of central black hole and
stellar cluster generates free energy, which is dissipated in collisions, and
maintains the thickness of the torus. A quantitative treatment for the torus in
the prototypical Seyfert 2 nucleus of NGC 1068 together with a radiative
transfer calculation for NIR re-emission from the torus is presented.
