碎片轨道的碰撞和热辐射模型：微行星的星族性质
Collisional and Thermal Emission Models of Debris Disks: Towards Planetesimal Population Properties
摘要：
围绕主序星的碎片盘被认为是来自于在早期时期吸积的小行星群，并在可能的行星形成过程中幸存下来。虽然碎片盘必须包含各种尺寸的固体-从大的星子到微小的尘埃颗粒-碎片盘的观测只对尺寸分布的尘埃端敏感。碎片盘的碰撞模型需要“爬上”碰撞级联的阶梯，从尘埃到母体，代表盘的主要质量库。我们已经使用我们的碰撞代码来生成一个类似太阳的恒星周围的五个磁盘，假设星子带在3，10，30，100，和200 AU的10倍的埃奇-柯伊伯带质量密度，并将它们演化为10 Gyr。随着适当的缩放规则，这有效地产生了一个三参数的参考盘集（初始质量，星子带的位置，年龄）。对于所有的磁盘，我们已经产生了光谱能量分布（SED），假设均匀的球形星状硅酸盐尘埃颗粒。生成的和实际观察到的SED之间的比较产生的星子属性（位置，总质量等）的估计。作为测试和这种方法的第一个应用，我们选择了五个磁盘周围的太阳类似的恒星与著名的SED。在四种情况下，我们用网格中两个圆盘的线性组合（一个3天文单位的“小行星带”和一个外部的“柯伊伯带”）再现了数据;在一种情况下，一个外部的组成部分就足够了。外层的组成部分与0.2-50个地球质量的“大柯伊伯带”（直径可达100公里）和半径为100-200 AU的“大柯伊伯带”相兼容。
英文摘要：
Debris disks around main-sequence stars are believed to derive from planetesimal populations that have accreted at early epochs and survived possible planet formation processes. While debris disks must contain solids in a broad range of sizes - from big planetesimals down to tiny dust grains - debris disk observations are only sensitive to the dust end of the size distribution. Collisional models of debris disks are needed to "climb up" the ladder of the collisional cascade, from dust towards parent bodies, representing the main mass reservoir of the disks. We have used our collisional code to generate five disks around a sun-like star, assuming planetesimal belts at 3, 10, 30, 100, and 200 AU with 10 times the Edgeworth-Kuiper-belt mass density, and to evolve them for 10 Gyr. Along with an appropriate scaling rule, this effectively yields a three-parametric set of reference disks (initial mass, location of planetesimal belt, age). For all the disks, we have generated spectral energy distributions (SEDs), assuming homogeneous spherical astrosilicate dust grains. A comparison between generated and actually observed SEDs yields estimates of planetesimal properties (location, total mass etc.). As a test and a first application of this approach, we have selected five disks around sun-like stars with well-known SEDs. In four cases, we have reproduced the data with a linear combination of two disks from the grid (an "asteroid belt" at 3 AU and an outer "Kuiper belt"); in one case a single, outer component was sufficient. The outer components are compatible with "large Kuiper belts" of 0.2-50 earth masses (in the bodies up to 100 km in size) with radii of 100-200 AU.
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