Abstract
Our current numerical work realised with the help of the HLRB II supercomputer focuses on the so-called Seyfert phenomenon. Whenever enough gas is accreted onto the central supermassive black holes of otherwise normal galaxies, their centres light up to become as bright as the stars of the whole galaxy. The main aim of this joint project is to understand the origin and evolution of the complex stellar, gaseous and dusty structures around supermassive black holes and how such activity cycles might be triggered and what consequences this has on the surrounding distribution of gas and dust. We mainly follow four areas of research: (i) star formation in the direct vicinity of supermassive black holes, (ii) radiative interaction of dust clouds in tori, (iii) multi-phase turbulence in obscuring tori and (iv) studying the connection between nuclear star formation and black hole feeding. This is done with the help of up-to-date numerical methods: high resolution grid based hydrodynamics codes (Pluto, Nirvana), highly adaptive SPH-codes (Gadget2) are developed further to include radiation pressure effects and a new code is developed to treat the radiation pressure interactions in an ensemble of dust clouds.
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