Models of dust and gas tori in active galactic nuclei
The goal of this thesis is to gain theoretical understanding of the distribution of dust and gas in the innermost parsecs of Active Galactic Nuclei. Unified schemes demand a circum-nuclear disk or "torus" to geometrically unify two separate classes of observed objects (face-on and edge-on...
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| Format: | Book/Monograph Thesis |
| Language: | English |
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2007
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| Online Access: | Resolving-System, kostenfrei, Volltext: http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-71865 Verlag, Volltext: http://archiv.ub.uni-heidelberg.de/volltextserver/volltexte/2007/7186 Verlag, Volltext: http://archiv.ub.uni-heidelberg.de/volltextserver/volltexte/2007/7186/pdf/phd_thesis_schartmann.pdf 
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| Author Notes: | Marc Schartmann |
| Summary: | The goal of this thesis is to gain theoretical understanding of the distribution of dust and gas in the innermost parsecs of Active Galactic Nuclei. Unified schemes demand a circum-nuclear disk or "torus" to geometrically unify two separate classes of observed objects (face-on and edge-on view onto the torus). In a multi-step approach, we work towards the establishment of realistic simulations of this massive and dense gas and dust reservoir, in order to be able to interpret near- and mid-infrared interferometric observations (MIDI, AMBER), which are able to resolve dust structures in the centres of Seyfert galaxies. In a first step, we investigate an analytical torus model (the so-called "Turbulent Torus Model") with the help of radiative transfer calculations and find gross agreement with large aperture, as well as high-resolution observations of Seyfert galaxies. However, the model SEDs show too pronounced silicate emission features in the face-on case. This can be overcome with the help of three-dimensional clumpy tori, calculated in a second step. Special emphasis is put on the differences of clumpy and continuous dust distributions, also concerning interferometric observations. In a further step, we apply hydrodynamic simulations to trace the evolution of a nuclear star cluster, which provides energy via discrete supernova explosions and mass from stellar mass loss... |
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| Physical Description: | Online Resource |