Modeling of radial and azimuthal structure in debris disks

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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.