Recently , high resolution observations with the help of the near-infrared adaptive optics integral field spectrograph SINFONI at the VLT proved the existence of massive and young nuclear star clusters in the centres of a sample of Seyfert galaxies .
With the help of high resolution hydrodynamical simulations with the PLUTO -code , we follow the evolution of such clusters , especially focusing on mass and energy feedback from young stars .
This leads to a filamentary inflow of gas on large scales ( tens of parsec ) , whereas a turbulent and very dense disc builds up on the parsec scale .
Here , we concentrate on the long-term evolution of the nuclear disc in NGC 1068 with the help of an effective viscous disc model , using the mass input from the large scale simulations and accounting for star formation in the disc .
This two-stage modelling enables us to connect the tens of parsec scale region ( observable with SINFONI ) with the parsec scale environment ( MIDI observations ) .
At the current age of the nuclear star cluster , our simulations predict disc sizes of the order of 0.8 to 0.9 pc , gas masses of 10 ^ { 6 } M _ { \odot } and mass transfer rates through the inner boundary of 0.025 M _ { \odot } /yr in good agreement with values derived from observations .