空间扩展碎片盘中的碰撞过程和尺寸分布
Collisional processes and size distribution in spatially extended debris discs
摘要：
我们提出了一个新的多环代码的碰撞发展扩展碎片盘的研究。我们的第一个目标是确认从单环系统中获得的结果，即“真实”碎片盘中的尺寸分布总是偏离理论碰撞平衡$dN\proptoR^{-3.5}dR$幂律，特别是在可观测粒子的关键尺寸范围内（<1厘米），在那里它显示出特有的波浪图案。我们还旨在研究碎片盘密度分布、散射光光度分布和SEDs如何受到碰撞和径向混合的耦合效应的影响，这是由于辐射压力影响小颗粒造成的。模拟了从微米级颗粒到50公里级颗粒的尺寸分布演化。该模型考虑了受辐射压力影响的小颗粒的关键影响。本文研究了半径为120 AU、初始面密度为$Σ(a)\propto a^α$的基准盘的碰撞演化。我们表明，该系统的径向延伸起着至关重要的作用：在大多数地区的碰撞和大小演变的尘埃是由偏心或未绑定的轨道上产生的小颗粒进一步内盘。小颗粒的空间分布强烈偏离初始分布，而包含系统大部分质量的较大物体仍然遵循初始分布。这有后果的散射光的径向配置文件，得到显着平坦，我们提出了一个经验法则追溯到大型看不见的母体从观察到的配置文件的分布。最后，我们提供了碰撞尺寸分布和碰撞时间尺度的经验公式，可用于未来的碎片盘建模。
英文摘要：
We present a new multi-annulus code for the study of collisionally evolving extended debris discs. We first aim to confirm results obtained for a single-annulus system, namely that the size distribution in "real" debris discs always departs from the theoretical collisional equilibrium $dN\proptoR^{-3.5}dR$ power law, especially in the crucial size range of observable particles (<1cm), where it displays a characteristic wavy pattern. We also aim at studying how debris discs density distributions, scattered light luminosity profiles, and SEDs are affected by the coupled effect of collisions and radial mixing due to radiation pressure affected small grains. The size distribution evolution is modeled from micron-sized grains to 50km-sized bodies. The model takes into account the crucial influence of radiation pressure-affected small grains. We consider the collisional evolution of a fiducial a=120AU radius disc with an initial surface density in $Σ(a)\propto a^α$. We show that the system's radial extension plays a crucial role: in most regions the collisional and size evolution of the dust is imposed by small particles on eccentric or unbound orbits produced further inside the disc. The spatial distribution of small grains strongly departs from the initial profile, while the bigger objects, containing most of the system's mass, still follow the initial distribution. This has consequences on the scattered--light radial profiles which get significantly flatter, and we propose an empirical law to trace back the distribution of large unseen parent bodies from the observed profiles. We finally provide empirical formula for the collisional size distribution and collision timescale that can be used for future debris disc modeling.
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