Chondrule formation during planetesimal accretion
Chondrule formation during planetesimal accretion
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DOI：
10.1016/j.epsl.2011.06.007
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发表时间：
2011-08-15
影响因子：
5.3
通讯作者：
Movshovitz, Naor
中科院分区：
文献类型：
--
作者：
Asphaug, Erik;Jutzi, Martin;Movshovitz, Naor
我们探讨的想法，大多数球粒形成的结果，低效的成对吸积，当熔融或部分熔融的小行星直径-30-100公里，类似的大小，碰撞的速度相当于他们的两体逃逸速度类似于100米/秒。虽然速度太慢，无法产生冲击波或破坏目标，但这些碰撞是混乱的，特别是在类似1 Ma的动力学激发之后。在SPH模拟中，我们发现，最里面的部分的弹丸减速进入目标，而其余的继续在大规模的片。从碰撞前的静水压力P-0（1-100 bar）卸载到星云中，熔融物与球粒大小的液滴的表面能达到平衡。碰撞后，通过光学厚片的膨胀来调节冷却。在小时-天的时间尺度上。大部分的金属片落在目标上进行再加工，其余的被分散。(C)2011爱思唯尔有限公司版权所有。
We explore the idea that most chondrules formed as a consequence of inefficient pairwise accretion, when molten or partly molten planetesimals -30-100 km diameter, similar in size, collided at velocities comparable to their two-body escape velocity similar to 100 m/s. Although too slow to produce shocks or disrupt targets, these collisions were messy, especially after similar to 1 Ma of dynamical excitation. In SPH simulations we find that the innermost portion of the projectile decelerates into the target, while the rest continues downrange in massive sheets. Unloading from pre-collision hydrostatic pressure P-0 similar to 1-100 bar into the nebula, the melt achieves equilibrium with the surface energy of chondrule-sized droplets. Cooling is regulated post collision by the expansion of the optically thick sheets. on a timescale of hours-days. Much of the sheet rains back down onto the target to be reprocessed; the rest is dispersed. (C) 2011 Elsevier B.V. All rights reserved.