Dynamik und Kinetik schmaler Staubringe

土星环系统包含许多狭窄的尘埃环，如F环、恩克间隙小环和卡西尼分区的几个小环。从先驱者号的数据（Cuzzi和Burns， 1988）可以得出结论，F环呈现出其独特的团块和扭曲的外观是由于嵌入在尘埃环中的一组看不见的小卫星带的引力作用和相互作用，卡西尼号任务的数据证实了这一情况（Murray et al, 2008）。在恩克裂口的中心尘埃环中也发现了非常相似的行为（Ferrari and Brahic, 1997; Hahn, 2006），在那里，一条嵌入的小卫星带被推测为潘轨道附近观测到的尘埃的主要来源。在这个项目中，我们将为这样一个卫星带的尘埃产生、动态演化和损失机制的动力学平衡建立一个模型。这一点到目前为止还没有研究过。详细的建模和与卡西尼号观测结果的比较将有助于限制尘埃产生的物理参数，尘埃的特性，以及卫星的分布和动态。通过这种方式，它将有可能在接近罗氏极限的尘埃环中识别出共同的物理过程——最后但并非最不重要的是——探测到尚未见过的嵌入小卫星。

Saturn s ring system contains a number of narrow dust rings, such as the F ring, the Encke Gap ringlets, and several ringlets in the Cassini division. Already from Pioneer data (Cuzzi and Burns, 1988) it was concluded that the F ring assumes its peculiar clumpy and twisted appearance due to the gravitational action and interaction of a belt of small unseen moons embedded in a dusty ring, a scenario confirmed by data from the Cassini mission (Murray et al., 2008). A very similar behavior is found for the central dusty ring in the Encke Gap (Ferrari and Brahic, 1997; Hahn, 2006) where the presence of a belt of small embedded moons has been conjectured to serve as main sources for the observed dust near Pan s orbit. In this project we will develop a model for the kinetic balance of dust production, dynamical evolution, and loss mechanisms for such a belt of moons. This has not been studied so far. Detailed modeling and comparison to Cassini observations will help to constrain the parameters of the physics of dust creation, the properties of the dust, as well as the distribution and dynamics of the moons. In this way it will be possible to identify common physical processes in dust rings near the Roche limit - and last but not least - to detect yet unseen embedded moonlets.