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Young chondrules in CB chondrites from a giant impact in the early Solar System

机译：早期太阳系的巨大影响使CB球粒陨石中的年轻球粒

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摘要

Chondrules, which are the major constituent of chondritic meteorites, are believed to have formed during brief, localized, repetitive melting of dust ( probably caused by shock waves(1,2)) in the protoplanetary disk around the early Sun. The ages of primitive chondrules(3-6) in chondritic meteorites indicate that their formation started shortly after that of the calcium-aluminium-rich inclusions (4,567.2 +/- 0.7 Myr ago) and lasted for about 3 Myr, which is consistent with the dissipation timescale for protoplanetary disks around young solar-mass stars(7). Here we report the Pb-207-Pb-206 ages of chondrules in the metal-rich CB (Bencubbin-like) carbonaceous chondrites Gujba (4,562.7 +/- 0.5 Myr) and Hammadah al Hamra 237 (4,562.8 +/- 0.9 Myr), which formed during a single-stage, highly energetic event(8-11). Both the relatively young ages and the single-stage formation of the CB chondrules are inconsistent with formation during a nebular shock wave(2). We conclude that chondrules and metal grains in the CB chondrites formed from a vapour-melt plume produced by a giant impact between planetary embryos after dust in the protoplanetary disk had largely dissipated. These findings therefore provide evidence for planet-sized objects in the earliest asteroid belt, as required by current numerical simulations of planet formation in the inner Solar System(12).
机译：软骨是陨石陨石的主要成分，据信是在早期太阳周围的原行星盘中短暂，局部，重复性地融化尘土（可能是由冲击波（1,2）引起）形成的。球粒陨石中原始软骨的年龄（3-6）表明其形成是在富含钙铝的包裹体（4,567.2 +/- 0.7 Myr之前）之后不久开始的，持续了约3 Myr，这与围绕年轻太阳质量恒星的原行星盘的耗散时间尺度（7）。在这里，我们报告了富含金属的CB（本本宾宾样）碳质球粒状长方石Gujba（4,562.7 +/- 0.5 Myr）和Hammadah al Hamra 237（4,562.8 +/- 0.9 Myr）中软骨的Pb-207-Pb-206年龄，它是在一个单阶段的，充满活力的事件中形成的（8-11）。相对年轻的年龄和CB软骨的单阶段形成都与星状冲击波期间的形成不一致（2）。我们得出的结论是，CB球粒陨石中的球状晶体和金属晶粒是由原行星盘中的尘埃大量消散后，由行星胚胎之间的巨大撞击所产生的蒸气熔​​体羽流形成的。因此，这些发现为最早的小行星带中行星大小的物体提供了证据，这是目前太阳系内部行星形成的数值模拟所要求的（12）。

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