The Physics of Galactic Nuclei

Marc Schartmann (), Christian Alig, Martin Krause and Andreas Burkert
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Marc Schartmann: Max-Planck-Institut für extraterrestrische Physik
Christian Alig: Max-Planck-Institut für extraterrestrische Physik
Martin Krause: Max-Planck-Institut für extraterrestrische Physik
Andreas Burkert: Max-Planck-Institut für extraterrestrische Physik

A chapter in High Performance Computing in Science and Engineering, Garching/Munich 2009, 2010, pp 359-370 from Springer

Abstract: 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.

Keywords: Black Hole; Star Formation; Smooth Particle Hydrodynamic; Accretion Disc; Radiation Pressure (search for similar items in EconPapers)
Date: 2010
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DOI: 10.1007/978-3-642-13872-0_30

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