隐藏在阴影中的II：作为系外行星标记的碰撞尘埃
Hiding in the Shadows II: Collisional Dust as Exoplanet Markers
摘要：
对最年轻的行星（过渡盘为$\sim$ 1- 1千万年）的观测将提高我们的行星形成模型的准确性。不幸的是，即使在理想的情况下，对这些行星的观测也是具有挑战性和耗时的。因此，我们建议确定一组标记，可以预先选择有前途的外行星托管候选磁盘。为此，进行了N体模拟，以研究嵌入木星质量的行星对周围微行星盘动力学的影响，以及由此产生的第二代碰撞尘埃。我们使用一个新的碰撞模型，允许星子的碎片和侵蚀，和灰尘大小的碎片模拟后处理步骤，包括非引力，由于恒星辐射和气体原行星盘。从我们的数值模拟合成图像显示，一个明亮的双环在850 $μ$ m的低偏心率的行星，而一个高偏心率的行星将产生一个典型的内环与不对称的磁盘。在第一代原始尘埃的存在下，这些标记在远离嵌入行星的轨道的地方很难被探测到，但在过渡盘中的行星起源的间隙内可以被探测到。
英文摘要：
Observations of the youngest planets ($\sim$1-10 Myr for a transitional disk) will increase the accuracy of our planet formation models. Unfortunately, observations of such planets are challenging and time-consuming to undertake even in ideal circumstances. Therefore, we propose the determination of a set of markers that can pre-select promising exoplanet-hosting candidate disks. To this end, N-body simulations were conducted to investigate the effect of an embedded Jupiter mass planet on the dynamics of the surrounding planetesimal disk and the resulting creation of second generation collisional dust. We use a new collision model that allows fragmentation and erosion of planetesimals, and dust-sized fragments are simulated in a post process step including non-gravitational forces due to stellar radiation and a gaseous protoplanetary disk. Synthetic images from our numerical simulations show a bright double ring at 850 $μ$m for a low eccentricity planet, whereas a high eccentricity planet would produce a characteristic inner ring with asymmetries in the disk. In the presence of first generation primordial dust these markers would be difficult to detect far from the orbit of the embedded planet, but would be detectable inside a gap of planetary origin in a transitional disk.
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