arXiv 2202.012412022-02astro-ph.EPastro-ph.SR

原行星盘的大星群研究：解释有无子结构的毫米尺度-光度关系

A large population study of protoplanetary disks: Explaining the millimeter size-luminosity relation with or without sub-structure

Apostolos Zormpas, Tilman Birnstiel, Giovanni P. Rosotti, Sean M. Andrews

备注：: Replaced with the published version in A&A. 19+11 pages, 11+10 figures
发表信息：: A&A 661, A66 (2022)
DOI：: 10.1051/0004-6361/202142046

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摘要：

最近对附近原行星盘的尘埃连续辐射进行的亚弧秒分辨率调查显示，盘的大小和光度之间存在很强的相关性。我们的目标是解释的起源（亚）毫米的大小-光度关系（SLR）之间的$68\%$有效半径（$r_{eff}$）的磁盘与其连续光度（$L_{mm}$），在一个简单的粘性吸积盘和辐射传输计算的气体和尘埃的演变模型。我们使用一个大的网格模型（$10^{5}$模拟）与行星间隙，不同的初始条件的关键参数。我们计算的磁盘连续辐射和有效半径的所有模型作为时间的函数。通过选择那些连续跟随SLR的模拟，我们可以推导出对模型输入参数的约束。我们证实了以前的结果，即模型的径向漂移区的光滑盘是兼容的所观察到的SLR（$L_{mm}\propto r_{eff}^{2}$），但只有光滑盘不能成为现实。我们表明，SLR是更广泛的人口，如果行星存在。然而，它们往往遵循与光滑圆盘不同的关系，这可能意味着在观察到的样品中存在光滑圆盘和亚结构圆盘的混合物。我们推导出一个SLR（$L_{mm}\propto r_{eff}^{5/4}$）的磁盘具有强的子结构。为了与SLR兼容，模型需要具有初始高磁盘质量（$\geq 2.5 \cdot 10^{-2}M_{\star}$）和低磁致伸缩参数$α$值（$\leq 10^{-3}$）。此外，我们发现，晶粒组成和孔隙度极大地影响磁盘的演变的尺寸-光度图，其中相对紧凑的晶粒，包括无定形碳的青睐。此外，一个均匀的光学厚盘与高的折射率（$0.9$），以下的SLR不能形成从一个进化的过程。

英文摘要：

Recent sub-arcsecond resolution surveys of the dust continuum emission from nearby protoplanetary disks showed a strong correlation between the sizes and luminosities of the disks. We aim to explain the origin of the (sub-)millimeter size-luminosity relation (SLR) between the $68\%$ effective radius ($r_{eff}$) of disks with their continuum luminosity ($L_{mm}$), with models of gas and dust evolution in a simple viscous accretion disk and radiative transfer calculations. We use a large grid of models ($10^{5}$ simulations) with and without planetary gaps, varying the initial conditions of the key parameters. We calculate the disk continuum emission and the effective radius for all models as a function of time. By selecting those simulations that continuously follow the SLR, we can derive constraints on the input parameters of the models. We confirm previous results that models of smooth disks in the radial drift regime are compatible with the observed SLR ($L_{mm}\propto r_{eff}^{2}$) but only smooth disks cannot be the reality. We show that the SLR is more widely populated if planets are present. However they tend to follow a different relation than smooth disks, potentially implying that a mixture of smooth and sub-structured disks are present in the observed sample. We derive a SLR ($L_{mm}\propto r_{eff}^{5/4}$) for disks with strong sub-structure. To be compatible with the SLR, models need to have an initially high disk mass ($\geq 2.5 \cdot 10^{-2}M_{\star}$) and low turbulence-parameter $α$ values ($\leq 10^{-3}$). Furthermore, we find that the grain composition and porosity drastically affects the evolution of disks on the size-luminosity diagram where relatively compact grains that include amorphous carbon are favoured. Moreover, a uniformly optically thick disk with high albedo ($0.9$) that follows the SLR cannot be formed from an evolutionary procedure.

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