Abstract Determining the origins of chondrule precursors is key to constraining how material migrated in the early Solar System. Chondrules that were only partially melted during their formation retain portions of their solid precursors, termed relict grains. By measuring the chemical and O-isotopic compositions of relict grains in chondrules from an unequilibrated ordinary chondrite (UOC), and Renazzo-like carbonaceous (CR) and Mighei-like carbonaceous (CM) chondrites we constrain their origins and discuss implications for disk transport within the first 4 million years of the Solar System. For all three chondrite groups, the chemical and O-isotopic compositions of dusty olivine grains are sometimes consistent with the reduction of type I (FeO-poor) and/or type II (FeO-rich) chondrules from the same meteorite group. However, other dusty olivine grains from the CM chondrites and the UOC are found to be xenocrysts that require an origin from a source distinct from the host meteorite. This material plausibly originated as fragments of earlier-formed chondrules from another chondrite group or of partially or fully differentiated planetesimals that migrated into an active chondrule-forming region. Multiple CM chondrite dusty olivine chondrules have O-isotope compositions that match those of UOC chondrule olivine (Δ17O ∼ 0‰), suggesting an origin from an UOC source. This implies that UOC chondrules and/or chondrule fragments migrated from the inner Solar System outwards to CM chondrite chondrule-forming region, likely beyond the orbit of Jupiter. These UOC chondrules or chondrule fragments could have migrated outwards in the protoplanetary disk before the formation of the Jupiter Gap, or

中文翻译：

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早期太阳系球粒碎片的向外迁移：岩石物质穿越木星间隙的 O 同位素证据？

摘要 确定球粒前体的起源是限制物质在早期太阳系中迁移的关键。在形成过程中仅部分熔化的球粒保留了部分固体前体，称为残余颗粒。通过测量来自未平衡的普通球粒陨石 (UOC) 和 Renazzo 类碳质 (CR) 和 Mighei 类碳质 (CM) 球粒陨石中残余颗粒的化学和 O 同位素组成，我们限制了它们的起源并讨论了对圆盘运输的影响在太阳系的前 400 万年内。对于所有三个球粒陨石群，尘土橄榄石颗粒的化学和 O 同位素组成有时与同一陨石群的 I 型（贫铁）和/或 II 型（富铁）球粒的还原一致。然而，来自 CM 球粒陨石和 UOC 的其他尘土飞扬的橄榄石颗粒被发现是异种晶体，需要来自不同于宿主陨石的来源。这种物质可能起源于来自另一个球粒陨石群的较早形成的球粒碎片，或者是迁移到活跃的球粒形成区域的部分或完全分化的星子碎片。多个 CM 球粒陨石尘埃橄榄石球粒具有与 UOC 球粒橄榄石 (Δ17O ∼ 0‰) 相匹配的 O 同位素组成，表明其起源于 UOC 来源。这意味着 UOC 球粒和/或球粒碎片从太阳系内部向外迁移到 CM 球粒陨石形成区域，可能超出了木星的轨道。