在蒸发的冰质星子周围的shock waves中通过动力学尘埃聚集的细粒边缘形成
Fine-grained rim formation via kinetic dust aggregation in shock waves around evaporating icy planetesimals
摘要：
细粒边缘（FGR）经常发现在原始陨石球粒周围。FGR的显著特征是其亚微米尺寸和无孔性质。球粒周围FGR的典型厚度为10- 100 $μ$ m。最近，一个新的想法被提出来解释FGR的起源：球粒和细小尘埃颗粒之间的高速碰撞，称为动力学尘埃聚集过程。实验研究表明，在真空中，当撞击速度约为0.1- 1 km/s时，（亚）微米尺寸的陶瓷颗粒可以粘附在陶瓷基底上。在这项研究中，我们研究的可能性FGR形成通过动力学尘埃聚集在球粒形成的冲击波。当未分化的冰质微行星产生冲击波时，由于冰质微行星的蒸发，细小的尘埃颗粒将从行星表面释放出来。我们考虑了冲击波阵面后面的球粒动力学，并基于简单的一维计算通过动力学尘埃聚集计算FGR的增长。我们发现，在蒸发的冰质星子周围的激波中，会形成厚度为10- 100 $μ$ m的无孔FGR。
英文摘要：
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.
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