Dynamik und Kinetik schmaler Staubringe

土星的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。已经从先驱者的数据（Cuzzi和Burns，1988）得出结论，F环由于嵌入尘埃环中的一组看不见的小卫星的引力作用和相互作用而呈现出其独特的clusiveness和扭曲的外观，卡西尼使命的数据证实了这一情景（Murray等人，2008年）。一个非常相似的行为被发现的中央尘埃环在恩克间隙（法拉利和Brahic，1997年;哈恩，2006年），其中存在的一个带的小嵌入卫星已被证实作为主要来源，观察到的尘埃附近的潘s轨道。在这个项目中，我们将开发一个模型的动力学平衡的尘埃生产，动力学演变，和损失机制，这样一个卫星带。这一点迄今尚未得到研究。详细的建模和与卡西尼观测的比较将有助于限制尘埃产生的物理参数，尘埃的性质以及卫星的分布和动力学。通过这种方式，将有可能确定罗氏极限附近尘埃环中的常见物理过程-最后但并非最不重要的是-检测尚未看到的嵌入式小卫星。

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.