论文标题
散射引起的强度降低：TW hya磁盘内部区域中的大质量含量很大
Scattering-induced intensity reduction: large mass content with small grains in the inner region of the TW Hya disk
论文作者
论文摘要
尘埃连续观测是限制原行星磁盘特性的最佳方法之一。最近的理论研究表明，毫米波长的尘埃散射可能会降低观察到的强度，从而导致灰尘质量低估。我们研究尘埃散射是否确实通过比较3、4、6、7和9频段的TW hya磁盘的Alma档案数据与通过辐射传递模拟获得的模型来降低了观察到的连续强度。我们发现，具有300 $ {\ rmμm} $尺寸的散射模型很好地再现了TW hya磁盘的中央部分的观察到的SED，而没有散射的模型也在绝对磁通的误差中也保持一致。为了解释频段3的强度，尘埃表面密度必须为$ \ sim $ 10 $ {\ rm g \，cm^{ - 2}} $在10 au中，散射的模型中的10 au，其质量比以前预测的高26倍。没有散射的模型需要的尘埃质量是散射模型的2.3倍，因为它需要较低的温度。在频段7处，散射的强度降低了$ \ sim $ 35％，这使磁盘看起来很薄，即使它是光学厚的。我们的研究表明，TW HYA磁盘仍然能够形成当前太阳系行星的巨型行星岩心。
Dust continuum observation is one of the best methods to constrain the properties of protoplanetary disks. Recent theoretical studies have suggested that the dust scattering at the millimeter wavelength potentially reduces the observed intensity, which results in an underestimate in the dust mass. We investigate whether the dust scattering indeed reduces the observed continuum intensity by comparing the ALMA archival data of the TW Hya disk at Band 3, 4, 6, 7 and 9 to models obtained by radiative transfer simulations. We find that the model with scattering by 300 ${\rm μm}$-sized grains well reproduces the observed SED of the central part of the TW Hya disk while the model without scattering is also consistent within the errors of the absolute fluxes. To explain the intensity at Band 3, the dust surface density needs to be $\sim$ 10 ${\rm g\,cm^{-2}}$ at 10 au in the model with scattering, which is 26 times more massive than previously predicted. The model without scattering needs 2.3 times higher dust mass than the model with scattering because it needs lower temperature. At Band 7, scattering reduces the intensity by $\sim$ 35% which makes the disk looks optically thin even though it is optically thick. Our study suggests the TW Hya disk is still capable of forming cores of giant planets at where the current solar system planets exist.
