The Geometry of Resonant Signatures in Debris Disks with Planets
The Geometry of Resonant Signatures in Debris Disks with Planets
复制标题
行星碎片盘中共振特征的几何形状
DOI：
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
M. Holman
中科院分区：
文献类型：
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作者：
M. Kuchner;M. Holman
使用简单的几何参数，我们画的各种共振结构的概述一个中等偏心率（e = 0.6）的单行星可以创建一个动态冷，光学薄尘埃盘。这一概述可以作为解释扰动碎片盘图像和推断造成扰动的行星动力学特性的关键。我们比较了太阳系尘埃云的共振几何与观测的尘埃云周围的织女星，波江座，北落师门。
Using simple geometrical arguments, we paint an overview of the variety of resonant structures a single planet with moderate eccentricity (e ≲ 0.6) can create in a dynamically cold, optically thin dust disk. This overview may serve as a key for interpreting images of perturbed debris disks and inferring the dynamical properties of the planets responsible for the perturbations. We compare the resonant geometries found in the solar system dust cloud with observations of dust clouds around Vega, ϵ Eridani, and Fomalhaut.