论文标题
通过动力学灰尘聚集在蒸发冰冷的行星周围的冲击波中的细颗粒边缘形成
Fine-grained rim formation via kinetic dust aggregation in shock waves around evaporating icy planetesimals
论文作者
论文摘要
细颗粒的边缘（FGRS）经常在原始软骨的软骨周围发现。 FGR的显着特征是它们的亚微米大小和非孔子性质。软骨周围的FGR的典型厚度为10--100美元$ $ m。最近，提出了一个新颖的想法，该想法是FGRS的起源：软骨和细粉尘粒之间的高速碰撞，称为动力学粉尘聚集过程。实验研究表明，当冲击速度大约在0.1--1 km/s的范围内时，（亚）微米大小的陶瓷颗粒可以在真空中粘在真空中。在这项研究中，我们研究了通过软骨形成的冲击波中的动力学灰尘聚集来形成FGR形成的可能性。当通过未分化的冰冷的行星产生冲击波时，由于冰冰行星的蒸发，将从行星表面释放细粉尘颗粒。我们考虑了电击锋后的软骨的动力学，并根据简单的一维计算通过动力学灰尘聚集来计算FGR的生长。我们发现，厚度为10--100 $ $ m的非孔FGR将在蒸发冰冷的行星周围以冲击波形成。
Fine-grained rims (FGRs) are frequently found around chondrules in primitive chondrites. The remarkable feature of FGRs is their submicron-sized and non-porous nature. The typical thickness of FGRs around chondrules is 10--100 $μ$m. Recently, a novel idea was proposed for the origin of FGRs: high-speed collisions between chondrules and fine dust grains called the kinetic dust aggregation process. Experimental studies revealed that (sub)micron-sized ceramic particles can stick to a ceramic substrate in a vacuum when the impact velocity is approximately in the range of 0.1--1 km/s. In this study, we examine the possibility of FGR formation via kinetic dust aggregation in chondrule-forming shock waves. When shock waves are created by undifferentiated icy planetesimals, fine dust grains would be released from the planetary surface due to evaporation of icy planetesimals. We consider the dynamics of chondrules behind the shock front and calculate the growth of FGRs via kinetic dust aggregation based on simple one-dimensional calculations. We found that non-porous FGRs with the thickness of 10--100 $μ$m would be formed in shock waves around evaporating icy planetesimals.
