由盘的不稳定性讨论气体巨星在诞生过程中富集和分异的可能性
On The Possibility of Enrichment and Differentiation in Gas Giants During Birth by Disk Instability
摘要：
我们调查岩石大小的固体和气体之间的耦合，在形成气体巨行星的大规模磁盘的外部区域的磁盘碎片。在这项研究中，我们使用三维辐射流体动力学模拟和模型固体颗粒的空间分布。我们假设总固体分数的一半是小颗粒，一半是大固体。前者完全被气体夹带并在盘中设置不透明度，而后者则允许响应气体阻力，并考虑气体上的反作用。为了探索气固相互作用的最大效应，我们首先考虑10厘米大小的颗粒。然后，我们比较这些结果与1公里大小的颗粒，探索低阻力制度的模拟。我们发现：（1）盘不稳定性行星有可能形成大的核心，由于气动捕获岩石大小的固体在螺旋臂破碎之前;（2）临时团块可以集中几十个$M_{\oplus}$固体在非常局部的区域之前，团块破裂;（3）永久团块的形成，即使在外盘，是依赖于粒度分布，即，不透明性;（4）盘中的非轴对称结构可以产生固气比大于1的盘区域;（5）固体分布可能影响碎裂过程;（6）原始气体巨星和原始棕矮星可以在H $_2$坍缩阶段之前作为差异化的物体开始;（7）引力不稳定盘中的旋臂能够阻止岩石大小的固体向内漂移，甚至将它们重新分配到更大的半径;以及（8）大的固体可以形成偏离气体螺旋臂的螺旋臂。我们的结论是，行星胚胎的形成可以强烈影响的固体在磁盘吸积的最早阶段的增长。
英文摘要：
We investigate the coupling between rock-size solids and gas during the formation of gas giant planets by disk fragmentation in the outer regions of massive disks. In this study, we use three-dimensional radiative hydrodynamics simulations and model solids as a spatial distribution of particles. We assume that half of the total solid fraction is in small grains and half in large solids. The former are perfectly entrained with the gas and set the opacity in the disk, while the latter are allowed to respond to gas drag forces, with the back reaction on the gas taken into account. To explore the maximum effects of gas-solid interactions, we first consider 10cm-size particles. We then compare these results to a simulation with 1 km-size particles, which explores the low-drag regime. We show that (1) disk instability planets have the potential to form large cores due to aerodynamic capturing of rock-size solids in spiral arms before fragmentation; (2) that temporary clumps can concentrate tens of $M_{\oplus}$ of solids in very localized regions before clump disruption; (3) that the formation of permanent clumps, even in the outer disk, is dependent on the grain-size distribution, i.e., the opacity; (4) that nonaxisymmetric structure in the disk can create disk regions that have a solids-to-gas ratio greater than unity; (5) that the solid distribution may affect the fragmentation process; (6) that proto-gas giants and proto-brown dwarfs can start as differentiated objects prior to the H$_2$ collapse phase; (7) that spiral arms in a gravitationally unstable disk are able to stop the inward drift of rock-size solids, even redistributing them to larger radii; and, (8) that large solids can form spiral arms that are offset from the gaseous spiral arms. We conclude that planet embryo formation can be strongly affected by the growth of solids during the earliest stages of disk accretion.
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