居住在薄碎片盘中的行星胚胎和微行星
Planetary embryos and planetesimals residing in thin debris disks
摘要：
我们考虑的限制居住在磁盘的天文台Microscopii，Beta Picture和北落师门的星子人口考虑到他们观察到的厚度和正常的磁盘不透明度。我们估计，半径为5，180和70公里的机构负责启动的碰撞级联占的尘埃生产的AU-Mic，β-Pic和北落师门的磁盘，分别在破裂半径从恒星的表面亮度曲线变化的斜率。假设这些盘是由引力搅拌加热的，那么需要半径为1000 km、面密度为0.01 g/cm ^2量级的更大天体来解释这些盘的厚度。两种大小的密度之间的比较表明，最大天体的大小分布比在柯伊伯带中观察到的要平坦。对于半径大于10公里的天体来说，AU Mic的圆盘需要最浅的尺寸分布，这表明圆盘包含了经历失控生长阶段的行星胚胎。
英文摘要：
We consider constraints on the planetesimal population residing in the disks of AU Microscopii, Beta Pictoris and Fomalhaut taking into account their observed thicknesses and normal disk opacities. We estimate that bodies of radius 5, 180 and 70 km are responsible for initiating the collisional cascade accounting for the dust production for AU-Mic, Beta-Pic and Fomalhaut's disks, respectively, at break radii from the star where their surface brightness profiles change slope. Larger bodies, of radius 1000km and with surface density of order 0.01 g/cm^2, are required to explain the thickness of these disks assuming that they are heated by gravitational stirring. A comparison between the densities of the two sizes suggests the size distribution in the largest bodies is flatter than that observed in the Kuiper belt. AU Mic's disk requires the shallowest size distribution for bodies with radius greater than 10km suggesting that the disk contains planetary embryos experiencing a stage of runaway growth.
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