Modeling of radial and azimuthal structure in debris disks

到目前为止，所有围绕主序星的碎片盘都是有结构的。该项目旨在在两个基本场景的框架下详细研究径向（环，内部间隙）和方位角结构（团块）。这两种方法都需要行星的存在，行星要么直接塑造尘埃分布，要么塑造尘埃母体的数量，从而也塑造它们产生的尘埃。我们建议扩展和改进这两种情况的模型。在这些模型的帮助下，我们将研究这两种机制的效率如何取决于负责结构的行星和星子的性质。结果将应用于解释几个已分辨圆盘的观测结构，并通过下一代仪器，如Herschel/PACS和Herschel/SPIRE， ALMA和JCMT/SCUBA2，对其远红外和亚毫米波长的可观测性进行估计。我们还将应用这些结果来预测我们太阳系的碎片盘，即埃奇沃斯-柯伊伯带中的尘埃分布。结果将提供给社区，并将有助于仪器科学规划和解释现有数据。最终，这个项目将有助于更好地了解碎片盘，并阐明行星系统的形成和演化。

All debris disks around main-sequence stars resolved so far are structured. This project aims at a detailed study of radial (rings, inner gaps) and azimuthal structure (clumps) in the framework of two basic scenarios. Both of them require the presence of a planet, which sculpts either dust distributions directly or populations of dust parent bodies and thus also the dust they produce. We propose to extend and improve our models of both scenarios. With the aid of these models, we will investigate, how the efficiency of both mechanisms depends on the properties of planets and planetesimals responsible for the structure. The results will be applied to interpret the observed structure in several resolved disks and to make estimates of its observability at far-IR and sub-mm wavelengths by next-generation instruments, such as Herschel/PACS and Herschel/SPIRE, ALMA, and JCMT/SCUBA2. We will also apply the results to predict the dust distribution in the debris disk of our own solar system, the Edgeworth-Kuiper belt. The results will be made available to the community and will help in the instrument science planning and interpretation of available data. Ultimately, this project could contribute to a better understanding of debris disks and shed light on the formation and evolution of planetary systems.