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<p>Enstatite chondrites-like impactors are proposed as key contributors to the proto-Earth and are believed to have undergone differentiation. However, this differentiation remains enigmatic: their small size precludes gravity-driven permeable flow, and enstatite exhibits a high melting temperature. Here, we report high-pressure melting experiments on EH3 chondrite, coupled with three-dimensional X-ray computed tomography, showing that more than 20% of silicate partial melting can enable efficient metal segregation. Thermodynamic simulations of EH chondrite-like embryos thermal evolution further demonstrate that heat from radioactive decay allows core formation only if embryos accreted within 1.4 Myr post-CAIs. In contrast, EH chondrite parent bodies formed later (1.92–2.0 Myr post-CAIs) with radii of 110–190 km. Our findings suggest two distinct evolutionary trajectories of EH chondrite-like embryos, providing constraints on core formation in small planetary embryos and fundamental references for the formation of planets in the early solar system.</p>

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Rapid accretion of enstatite chondrite (EH)-like embryos as impactors for the proto-Earth

  • 期刊论文

  • 出版模式：

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  • 发表日期：

    2026年7月25日

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  • Qiong Li,
  • Wei Du,
  • Jing Yang,
  • Chuan Zhang,
  • Di Yao,
  • Keqing Zong,
  • Feiyang Chen,
  • Yonggang Wang,
  • Yun Liu

摘要

Enstatite chondrites-like impactors are proposed as key contributors to the proto-Earth and are believed to have undergone differentiation. However, this differentiation remains enigmatic: their small size precludes gravity-driven permeable flow, and enstatite exhibits a high melting temperature. Here, we report high-pressure melting experiments on EH3 chondrite, coupled with three-dimensional X-ray computed tomography, showing that more than 20% of silicate partial melting can enable efficient metal segregation. Thermodynamic simulations of EH chondrite-like embryos thermal evolution further demonstrate that heat from radioactive decay allows core formation only if embryos accreted within 1.4 Myr post-CAIs. In contrast, EH chondrite parent bodies formed later (1.92–2.0 Myr post-CAIs) with radii of 110–190 km. Our findings suggest two distinct evolutionary trajectories of EH chondrite-like embryos, providing constraints on core formation in small planetary embryos and fundamental references for the formation of planets in the early solar system.