  Recently, the MID-infrared Interferometric instrument (MIDI) at the VLTI has
shown that dust tori in the two nearby Seyfert galaxies NGC 1068 and the
Circinus galaxy are geometrically thick and can be well described by a thin,
warm central disk, surrounded by a colder and fluffy torus component. By
carrying out hydrodynamical simulations with the help of the TRAMP code (Klahr
et al. 1999), we follow the evolution of a young nuclear star cluster in terms
of discrete mass-loss and energy injection from stellar processes. This
naturally leads to a filamentary large scale torus component, where cold gas is
able to flow radially inwards. The filaments open out into a dense and very
turbulent disk structure. In a post-processing step, we calculate observable
quantities like spectral energy distributions or images with the help of the 3D
radiative transfer code MC3D (Wolf 2003). Good agreement is found in
comparisons with data due to the existence of almost dust-free lines of sight
through the large scale component and the large column densities caused by the
dense disk.
