论文标题
在巨人的阴影中碰撞：气体巨人生长和迁移期间的行星碰撞
Colliding in the shadows of giants: Planetesimal collisions during the growth and migration of gas giants
论文作者
论文摘要
巨型行星迁移是行星系统进化中的重要现象。最近的作品表明，巨型行星的生长和迁移可以塑造小行星带，但是这些作品并未考虑行星模拟之间的相互作用。我们已经计算了在气体巨大生长和迁移期间，包括行星星球碰撞在内的行星磁盘的演变。这些碰撞的数字，位置和影响速度取决于特定的生长和迁移路径。我们发现，仅巨型行星的增长对冲击速度的影响很小，而大多数因增长巨人而散布的地球上的大多数行星在增长期间不会彼此碰撞。相比之下，我们发现巨型行星迁移会引起行星可能之间的大量高速碰撞。这些影响具有足够的速度，可导致地球上的水冰和硅酸盐成分引起冲击引起的蒸发，并引起人体灾难性破坏。撞击碎片可能会形成新物体。碰撞进化可通过巨型行星的生长和迁移来降低行星植入小行星带的效率。将通过碰撞处理植入小行星带植入小行星带的一小部分。我们确定了行星积聚模型中未考虑的行星碰撞的重要后果。巨型行星迁移期间高速碰撞的流行率及其与陨石的特性的潜在联系以及软骨的形成使影响蒸发成为至关重要的现象。蒸发行星成分的后果需要进一步的详细研究。需要新的碰撞结果模型，以实现星云内的影响，并且需要新的行星形成模型。
Giant planet migration is an important phenomenon in the evolution of planetary systems. Recent works have shown that giant planet growth and migration can shape the asteroid belt, but these works have not considered interactions between planetesimals. We have calculated the evolution of planetesimal disks, including planetesimal-planetesimal collisions, during gas giant growth and migration. The numbers, locations, and impact velocities of these collisions depend on the specific growth and migration path. We find that giant planet growth alone has little effect on impact velocities, and most of the planetesimals scattered by growing giants do not undergo collisions with each other during the growth period. In contrast, we find that giant planet migration induces large numbers of high velocity collisions between planetesimals. These impacts have sufficient velocities to cause shock-induced vaporization for both water ice and silicate components of planetesimals, and to cause catastrophic disruption of the bodies. New bodies may form from impact debris. Collisional evolution reduces the efficiency of planetesimal implantation into the asteroid belt via giant planet growth and migration. A small fraction of the largest planetesimals implanted into the asteroid belt would have been processed via collisions. We identify important consequences of planetesimal collisions that have not been considered in planet accretion models. The prevalence of high velocity collisions during giant planet migration, and their potential links to the properties of meteorites, and the formation of chondrules, makes impact vaporization a critically important phenomenon. The consequences of vaporizing planetesimal constituents require further detailed study. New collision outcome models for impacts within the nebula, and models for new planetesimal formation are needed.
