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Models of the η Corvi Debris Disk from the Keck Interferometer, Spitzer, and Herschel

机译：来自Keck干涉仪，Spitzer和Herschel的ηCorvi碎片盘的模型

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Debris disks are signposts of analogs to small-body populations of the solar system, often, however, with much higher masses and dust production rates. The disk associated with the nearby star η Crv is especially striking, as it shows strong mid- and far-infrared excesses despite an age of ~1.4 Gyr. We undertake constructing a consistent model of the system that can explain a diverse collection of spatial and spectral data. We analyze Keck Interferometer Nuller measurements and revisit Spitzer and additional spectrophotometric data, as well as resolved Herschel images, to determine the dust spatial distribution in the inner exozodi and in the outer belt. We model in detail the two-component disk and the dust properties from the sub-AU scale to the outermost regions by fitting simultaneously all measurements against a large parameter space. The properties of the cold belt are consistent with a collisional cascade in a reservoir of ice-free planetesimals at 133 AU. It shows marginal evidence for asymmetries along the major axis. KIN enables us to establish that the warm dust consists of a ring that peaks between 0.2 and 0.8 AU. To reconcile this location with the ~400 K dust temperature, very high albedo dust must be invoked, and a distribution of forsterite grains starting from micron sizes satisfies this criterion, while providing an excellent fit to the spectrum. We discuss additional constraints from the LBTI and near-infrared spectra, and we present predictions of what James Webb Space Telescope can unveil about this unusual object and whether it can detect unseen planets.
机译：碎片盘是类似太阳系小体种群的路标，但是它们通常具有更高的质量和更高的粉尘产生率。与附近恒星ηCrv相关的圆盘特别引人注目，因为尽管年龄约为1.4吉尔，但仍显示出强烈的中红外和远红外过量。我们承诺构建一个系统的一致模型，该模型可以解释空间和光谱数据的各种集合。我们分析了Keck干涉仪Nuller的测量结果，并再次访问了Spitzer和其他分光光度数据，以及解析的Herschel图像，以确定内部exozodi和外部带中的粉尘空间分布。我们通过对所有参数同时拟合较大的参数空间，详细建模了两分量磁盘和从亚澳大利亚尺度到最外层区域的粉尘特性。冷带的性质与133 AU的无冰小行星储层中的碰撞级联一致。它显示了沿主轴不对称的边际证据。 KIN使我们能够确定，温暖的灰尘由一个峰值介于0.2到0.8 AU之间的环组成。为了使该位置与〜400 K的粉尘温度保持一致，必须调用非常高的反照率粉尘，并且从微米尺寸开始的镁橄榄石晶粒分布可以满足该标准，同时又能很好地适应光谱。我们讨论了来自LBTI和近红外光谱的其他限制，并提出了关于詹姆斯·韦伯太空望远镜可以揭露该不寻常物体的预测，以及它是否可以探测到看不见的行星。

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