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Gas and dust structures in protoplanetary disks hosting multiple planets

机译：拥有多个行星的原行星盘中的气体和尘埃结构

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Context. Transition disks have dust-depleted inner regions and may represent an intermediate step of an on-going disk dispersal process, where planet formation is probably in progress. Recent millimetre observations of transition disks reveal radially and azimuthally asymmetric structures, where micron- and millimetre-sized dust particles may not spatially coexist. These properties can be the result of particle trapping and grain growth in pressure bumps originating from the disk interaction with a planetary companion. The multiple features observed in some transition disks, such as SR 21, suggest the presence of more than one planet. Aims. We aim to study the gas and dust distributions of a disk hosting two massive planets as a function of different disk and dust parameters. Observational signatures, such as spectral energy distributions, sub-millimetre, and polarised images, are simulated for various parameters. Methods. Two dimensional hydrodynamical and one dimensional dust evolution numerical simulations are performed for a disk interacting with two massive planets. Adopting the previously determined dust distribution, and assuming an axisymmetric disk model, radiative transfer simulations are used to produce spectral energy distributions and synthetic images in polarised intensity at 1.6 μm and sub-millimetre wavelengths (850 μm). We analyse possible scenarios that can lead to gas azimuthal asymmetries. Results. We confirm that planets can lead to particle trapping, although for a disk with high viscosity (αturb = 10-2), the planet should be more massive than 5 MJup and dust fragmentation should occur with low efficiency (vf ~ 30 m s-1). This will lead to a ring-like feature as observed in transition disks in the millimetre. When trapping occurs, we find that a smooth distribution of micron-sized grains throughout the disk, sometimes observed in scattered light, can only happen if the combination of planet mass and turbulence is such that small grains are not fully filtered out. A high disk viscosity (αturb = 10-2) ensures a replenishment of the cavity in micron-sized dust, while for lower viscosity (αturb = 10-3), the planet mass is constrained to be less than 5 MJup. In these cases, the gas distribution is likely to show low-amplitude azimuthal asymmetries caused by disk eccentricity rather than by long-lived vortices.
机译：上下文。过渡盘的内部区域充满了灰尘，可能代表正在进行的盘扩散过程的中间步骤，在此过程中可能正在形成行星。最近对过渡盘的毫米波观测揭示了径向和方位角的不对称结构，其中微米级和毫米级的尘埃颗粒可能在空间上不共存。这些属性可能是由于磁盘与行星伴侣相互作用而导致的压力颠簸中的颗粒捕集和晶粒长大的结果。在某些过渡盘（例如SR 21）中观察到的多种特征表明存在一个以上的行星。目的我们旨在研究包含两个大质量行星的磁盘的气体和尘埃分布，作为不同磁盘和尘埃参数的函数。针对各种参数模拟观察信号，例如光谱能量分布，亚毫米和偏振图像。方法。对与两个大质量行星相互作用的盘进行了二维流体动力学和一维除尘数值模拟。采用先前确定的粉尘分布，并假设轴对称盘模型，使用辐射转移模拟来产生光谱能量分布和极化强度为1.6μm和亚毫米波长（850μm）的合成图像。我们分析了可能导致气体方位角不对称的可能情况。结果。我们确认，尽管对于具有高粘度（αturb= 10-2）的圆盘，行星应大于5 MJup，并且应以低效率（vf〜30 m s-1）发生粉尘破碎，但行星仍可导致粒子捕获。 ）。如在毫米的过渡盘中所观察到的，这将导致环形特征。当捕获发生时，我们发现，只有当行星质量和湍流的结合使得小颗粒没有被完全滤出时，才能在整个磁盘上均匀地分布微米级颗粒，有时在散射光下观察到。较高的圆盘粘度（αturb= 10-2）可确保在微米级粉尘中补充腔体，而对于较低的粘度（αturb= 10-3），行星质量被限制为小于5 MJup。在这些情况下，气体分布可能显示出由盘偏心而不是由长寿命的涡流引起的低振幅方位角不对称性。

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