THE SPIRAL WAVE INSTABILITY INDUCED BY A GIANT PLANET. I. PARTICLE STIRRING IN THE INNER REGIONS OF PROTOPLANETARY DISKS
THE SPIRAL WAVE INSTABILITY INDUCED BY A GIANT PLANET. I. PARTICLE STIRRING IN THE INNER REGIONS OF PROTOPLANETARY DISKS
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DOI：
10.3847/1538-4357/833/2/126
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发表时间：
2016-10
期刊：
影响因子：
--
通讯作者：
J. Bae;R. Nelson;L. Hartmann
中科院分区：
文献类型：
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作者：
J. Bae;R. Nelson;L. Hartmann
我们最近表明，在吸积盘中传播的螺旋密度波可以通过与惯性波（或在浮力重要时的惯性波）共振耦合并将能量传递给惯性波对而经历参数不稳定性。在本文中，我们执行无粘三维全球流体动力学模拟，以检查这种不稳定性在原行星盘中由木星质量的行星驱动的螺旋波上的增长和后果。我们发现螺旋波通过螺旋波不稳定性（SWI）不稳定，产生流体动力湍流和持续的径向交替垂直流动，这些流动似乎与长波惯性模式有关。在区间中，Rp表示行星轨道的半长轴（假设为5au），与湍流相关的估计垂直扩散率的特征为。对于这里考虑的圆盘模型，扩散速率是这样的，大小可达几厘米的颗粒在第一个压力尺度高度内垂直混合。这表明，巨行星发射的螺旋波的不稳定性可以使固体颗粒和痕量化学物质从中间面明显分散。在行星形成模型中，连续的局部生产球粒/鹅卵石发生在Myr时间尺度上，为这些天体上的鹅卵石吸积提供原料，这种固体颗粒的搅拌可能会增加时间限制：行星胚胎和大型小行星必须在气态巨行星形成之前形成，否则SWI将显著降低球粒/鹅卵石的吸积效率。
We have recently shown that spiral density waves propagating in accretion disks can undergo a parametric instability by resonantly coupling with and transferring energy into pairs of inertial waves (or inertial-gravity waves when buoyancy is important). In this paper, we perform inviscid three-dimensional global hydrodynamic simulations to examine the growth and consequence of this instability operating on the spiral waves driven by a Jupiter-mass planet in a protoplanetary disk. We find that the spiral waves are destabilized via the spiral wave instability (SWI), generating hydrodynamic turbulence and sustained radially alternating vertical flows that appear to be associated with long wavelength inertial modes. In the interval , where Rp denotes the semimajor axis of the planetary orbit (assumed to be 5 au), the estimated vertical diffusion rate associated with the turbulence is characterized by . For the disk model considered here, the diffusion rate is such that particles with sizes up to several centimeters are vertically mixed within the first pressure scale height. This suggests that the instability of spiral waves launched by a giant planet can significantly disperse solid particles and trace chemical species from the midplane. In planet formation models where the continuous local production of chondrules/pebbles occurs over Myr timescales to provide a feedstock for pebble accretion onto these bodies, this stirring of solid particles may add a time constraint: planetary embryos and large asteroids have to form before a gas giant forms in the outer disk, otherwise the SWI will significantly decrease the chondrule/pebble accretion efficiency.