论文标题
Protoplanet诱导的三维气流对卵石积聚的影响$ \ rm \，i \ hspace { - 。1EM} i \，$。逆风政权
Influences of protoplanet-induced three-dimensional gas flow on pebble accretion $\rm\,I\hspace{-.1em}I\,$. Headwind regime
论文作者
论文摘要
卵石积聚是行星形成的主要理论之一。空气动力学的小颗粒（称为卵石）受气流高度影响。嵌入原星盘中的生长行星会诱导三维（3D）气流。在我们先前的研究中，我们专注于卵石积聚的剪切状态，并研究了行星诱导的气流对卵石积聚的影响。在论文I中，我们发现与未扰动的流动相比，卵石吸积在行星诱导的气流中效率低下，特别是当$ {\ rm st} \ rm st} \ lysSim10^{ - 3} $时，st是st stokes数字。遵循论文I，我们研究了行星诱导的气流对卵石积聚的影响。我们认为气体的逆风。在本研究中，我们将研究扩展到了卵石积聚的逆风状态。假设有一个非等温的，无粘的亚易生膜磁盘，我们在球形极地网格上执行3D流体动力学模拟，该网格的行星具有无量纲的质量，$ m = r _ {\ rm bondi}/h $，位于其中心，其中$ r _ {\ rm bondi} $ h $和$ h $和$ h $ radious and是bondi rade的量然后，我们使用流体动力学模拟数据来数字整合3D中卵石运动的方程。将我们的结果与磁盘中的湍流强度和卵石大小相结合，我们得出结论，行星诱导的气流仍然可以在行星形成的早期阶段卵石积聚。由于行星诱导的气流而导致的卵石积聚的抑制仅发生在行星形成的后期，尤其是在磁盘的内部区域。这可能有助于解释系外行星的分布和太阳系的架构，它们的内部和大型外行星都很小。
Pebble accretion is one of the major theories in planet formation. Aerodynamically small particles, called pebbles, are highly affected by the gas flow. A growing planet embedded in a protoplanetary disk induces three-dimensional (3D) gas flow. In our previous study, Paper I, we focused on the shear regime of pebble accretion, and investigated the influence of planet-induced gas flow on pebble accretion. In Paper I, we found that pebble accretion is inefficient in the planet-induced gas flow compared to that in the unperturbed flow, in particular when ${\rm St}\lesssim10^{-3}$, where St is the Stokes number. Following Paper I, we investigate the influence of planet-induced gas flow on pebble accretion. We consider the headwind of the gas, which is not included in Paper I. We extend our study to the headwind regime of pebble accretion in this study. Assuming a nonisothermal, inviscid sub-Keplerian gas disk, we perform 3D hydrodynamical simulations on the spherical polar grid which has a planet with the dimensionless mass, $m=R_{\rm Bondi}/H$, located at its center, where $R_{\rm Bondi}$ and $H$ are the Bondi radius and the disk scale height. We then numerically integrate the equation of motion of pebbles in 3D using hydrodynamical simulation data. Combining our results with the spacial variety of turbulence strength and pebble size in a disk, we conclude that the planet-induced gas flow still allows for pebble accretion in the early stage of planet formation. Suppression of pebble accretion due to the planet-induced gas flow occurs only in the late stage of planet formation, in particular in the inner region of the disk. This may be helpful to explain the distribution of exoplanets and the architecture of the Solar System, both of which have small inner and large outer planets.
