AU Microscopii碎片盘：多波长成像和建模
The AU Microscopii Debris Disk: Multiwavelength Imaging and Modeling
摘要：
主序星周围的碎片盘是由看不见的母体的侵蚀和蒸发产生的。显微镜座AU（GJ 803）是一个在不同光谱类型的盘演化背景下进行研究的引人注目的对象，因为它是一个M矮星，其近边盘可以直接与它的A5 V兄弟β Pic进行比较。我们用Keck II望远镜和自适应光学在近红外JHK波段高分辨率地分辨了8-60 AU的星盘，并发展了一种新的数据处理技术，用于去除恒星的点扩散函数。对于某些半径，盘中平面中的点源检测灵敏度比远离盘的区域低一个量级以上。我们在近红外波段测量了蓝色，并确认了内盘子结构的存在。一些结构特征表现出波长依赖的位置。通过模拟推断了盘的结构和颗粒组成特征。我们的方式，补充以前的工作的灰尘分布的建模。使用Monte Carlo辐射转移代码，我们比较了一个相对简单的模型的多孔颗粒的分布，一个广泛的数据集，同时拟合中面表面亮度分布和光谱能量分布。我们的模型证实，大规模的磁盘架构是一致的详细模型的稳态晶粒动力学。在这里，35-40天文单位的母体带负责产生尘埃，然后被恒星风和辐射压力向外吹。我们推断在外部区域中存在非常小的颗粒，其尺寸低至~0.05微米。这些大小与恒星质量损失率Mdot_* << 10^2 Mdot_sun一致。
英文摘要：
(abridged) Debris disks around main sequence stars are produced by the erosion and evaporation of unseen parent bodies. AU Microscopii (GJ 803) is a compelling object to study in the context of disk evolution across different spectral types, as it is an M dwarf whose near edge-on disk may be directly compared to that of its A5V sibling beta Pic. We resolve the disk from 8-60 AU in the near-IR JHK' bands at high resolution with the Keck II telescope and adaptive optics, and develop a novel data reduction technique for the removal of the stellar point spread function. The point source detection sensitivity in the disk midplane is more than a magnitude less sensitive than regions away from the disk for some radii. We measure a blue color across the near-IR bands, and confirm the presence of substructure in the inner disk. Some of the structural features exhibit wavelength-dependent positions. The disk architecture and characteristics of grain composition are inferred through modeling. We approach the modeling of the dust distribution in a manner that complements previous work. Using a Monte Carlo radiative transfer code, we compare a relatively simple model of the distribution of porous grains to a broad data set, simultaneously fitting to midplane surface brightness profiles and the spectral energy distribution. Our model confirms that the large-scale architecture of the disk is consistent with detailed models of steady-state grain dynamics. Here, a belt of parent bodies from 35-40 AU is responsible for producing dust that is then swept outward by the stellar wind and radiation pressures. We infer the presence of very small grains in the outer region, down to sizes of ~0.05 micron. These sizes are consistent with stellar mass-loss rates Mdot_* << 10^2 Mdot_sun.
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