Investigating dust trapping in transition disks with millimeter-wave polarization
Investigating dust trapping in transition disks with millimeter-wave polarization
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利用毫米波偏振研究过渡盘中的灰尘捕集
DOI：
10.1051/0004-6361/201628637
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
Birnstiel
中科院分区：
文献类型：
--
作者：
Kataoka;Pinilla;Dullemond;Henning;Birnstiel
背景已经观测到空间分辨的极化(亚)毫米辐射，例如在HL Tau周围的原行星盘中。磁性排列的颗粒通常被解释为偏振源。然而，具有足够高反照率的大尘埃颗粒的自散射是另一种极化机制，它正在成为一种不依赖于光谱指数的强制方法来限制原行星盘中尘埃颗粒的尺寸。目的研究当巨行星在盘中打开缺口时，在过渡盘中提出的尘埃捕集场景中毫米波长的尘埃极化。我们研究了特征偏振模式及其与盘倾角、尘埃大小演化、行星位置和观测波长的关系。方法将行星-盘相互作用的二维流体力学模拟与自洽尘埃增长模型相结合。这些与尺寸相关的尘埃密度分布被用于后续的三维辐射传输计算，以预测由于散射热发射而导致的ALMA波段的偏振度。结果尘埃自散射已被证明是产生偏振毫米波辐射的一种可行机制。我们发现，尘埃演化1 MYR后，带有行星间隙的圆盘的偏振图样呈现出独特的三环结构。两个狭窄的内环位于行星间隙边缘。第三个更宽的偏振环位于外盘中，超过100 Au。为了增加观测波长，所有三个环的位置都略有改变，其中最内和最外的环向内移动。当比较ALMA带3、6和7的结果时，这一距离是可以检测到的。在最高极化强度区域内，极化矢量定向于方位方向。对于倾斜的圆盘，磁通梯度引起的极化和倾斜引起的四极极化之间存在相互作用。对于中等倾斜的过渡盘，在λ=3.1 mm(带3)处偏振度高达~2%，远高于未来ALMA观测的探测下限。
ContextSpatially resolved polarized (sub-)mm emission has been observed for example in the protoplanetary disk around HL Tau. Magnetically aligned grains are commonly interpreted as the source of polarization. However, self-scattering by large dust grains with a high enough albedo is another polarization mechanism, which is becoming a compelling method independent of the spectral index to constrain the dust grain size in protoplanetary disks.AimsWe study the dust polarization at mm wavelengths in the dust trapping scenario proposed for transition disks, when a giant planet opens a gap in the disk. We investigate the characteristic polarization patterns and their dependence on disk inclination, dust size evolution, planet position, and observing wavelength.MethodsWe combine two-dimensional hydrodynamical simulations of planet-disk interactions with self-consistent dust growth models. These size-dependent dust density distributions are used for follow-up three-dimensional radiative transfer calculations to predict the polarization degree at ALMA bands due to scattered thermal emission.ResultsDust self-scattering has been proven to be a viable mechanism for producing polarized mm-wave radiation. We find that the polarization pattern of a disk with a planetary gap after 1 Myr of dust evolution shows a distinctive three-ring structure. Two narrow inner rings are located at the planet gap edges. A third wider ring of polarization is situated in the outer disk beyond 100 au. For increasing observing wavelengths, all three rings change their position slightly, where the innermost and outermost rings move inward. This distance is detectable when comparing the results at ALMA bands 3, 6, and 7. Within the highest polarized intensity regions the polarization vectors are oriented in the azimuthal direction. For an inclined disk there is an interplay between polarization originating from a flux gradient and inclination-induced quadrupole polarization. For intermediate inclined transition disks, the polarization degree is as high as ~2% atλ= 3.1 mm (band 3), which is well above the detection limit of future ALMA observations.
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DOI：
10.1051/0004-6361/201323176
发表时间：
2014-07
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
--
作者：
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通讯作者：
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DOI：
--
发表时间：
2015
期刊：
影响因子：
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作者：
S. Casassus;S. Marino;S. Pérez;P. Roman;A. Dunhill;P. Armitage;J. Cuadra;A. Wootten;G. V. D. Plas;L. Cieza;V. Moral;V. Christiaens;M. Montesinos
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DOI：
--
发表时间：
2014
期刊：
影响因子：
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作者：
Sebastián Marino;S. Pérez;S. Casassus
通讯作者：
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书评 - 宇宙的结构和演化 - 相对论天体物理学 - V.2
DOI：
--
发表时间：
1984
期刊：
影响因子：
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作者：
Y. Zeldovich;I. Novikov
通讯作者：
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