Chondrule collisions in shock waves
Chondrule collisions in shock waves
复制标题
冲击波中的球粒碰撞
DOI：
10.1111/j.1945-5100.2006.tb00526.x
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发表时间：
2006
影响因子：
2.2
通讯作者：
F. Ciesla
中科院分区：
文献类型：
--
作者：
F. Ciesla
翻译后摘要-详细的数值模型表明，太阳星云冲击波将能够热处理陨石球粒的方式是符合实验的限制。然而，最近有人认为，在冲击波阵面后面不同大小的球粒之间产生的高相对速度将导致高能碰撞，这将在球粒被加工时摧毁它们，而不是将它们保存下来并入陨石母体。在这里，这些碰撞的结果是定量探讨使用一个简单的解析表达式的粘性耗散的碰撞能量在液体层。它表明，熔融球粒可以生存的碰撞速度高达几百米每秒。研究还表明，在给定的冲击波中，球粒的热演化随球粒尺寸的变化而变化，这可能允许在给定的冲击波中形成不同纹理的球粒。虽然需要实验来进一步限制这项工作中使用的参数，但这些计算表明，冲击波后碰撞的预期结果与陨石中观察到的结果一致。
Abstract— Detailed numerical models have shown that solar nebula shock waves would be able to thermally process chondrules in a way that is consistent with experimental constraints. However, it has recently been argued that the high relative velocities that would be generated between chondrules of different sizes immediately behind the shock front would lead to energetic collisions that would destroy the chondrules as they were processed rather than preserving them for incorporation into meteorite parent bodies. Here the outcome of these collisions is quantitatively explored using a simple analytic expression for the viscous dissipation of collisional energy in a liquid layer. It is shown that molten chondrules can survive collisions at velocities as high as a few hundred meters per second. It is also shown that the thermal evolution of chondrules in a given shock wave varies with chondrule size, which may allow chondrules of different textures to form in a given shock wave. While experiments are needed to further constrain the parameters used in this work, these calculations show that the expected outcomes from collisions behind shock waves are consistent with what is observed in meteorites.