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 join into a dense and very turbulent disk structure. In a post-processing step, we calculate spectral energy distributions and images with the 3D radiative transfer code MC3D Wolf (2003) and compare them to observations. Turbulence in the dense disk component is investigated in a separate project.
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机译：最近，VLTI中红外干涉仪（MIDI）显示了两个附近的SEYFERT GALAXIES NGC 1068和循环星系中的灰尘托在几何上厚，可以通过薄，温暖的中央盘进行很好的描述，由a包围较冷，蓬松的花齿组件。通过在Tramp代码的帮助下进行流体动力模拟（Klahr等人1999），我们在恒星过程中的离散质量损失和能量注入方面遵循年轻核星座的演变。这自然地导致丝状大规模的圆环组件，其中冷气能够径向向内流动。丝绸加入密集，湍流的磁盘结构。在后处理步骤中，我们计算使用3D辐射传输代码MC3D狼（2003）的光谱能量分布和图像，并将它们与观察结果进行比较。在单独的项目中研究了密集盘组件中的湍流。
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