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Updated: Jan 8, 2026

Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas

Experimental Methods of Dust Charging and Mobilization on Surfaces with Exposure to Ultraviolet Radiation or Plasmas

Published on: April 3, 2018

嫦娥五号着陆区表层土厚度推断的月球小型撞击体通量增加

Mingwei Zhang¹, Bojun Jia^1,2, Vincent R Eke³

¹Institute of Remote Sensing and Geographical Information System, School of Earth and Space Sciences, Peking University, Beijing, China.

Nature communications

|December 22, 2025

Abstract:

Knowledge of the small impactor flux on the Moon can provide critical insights into lunar geological evolution and the dynamics of the inner solar system. However, it cannot be directly deciphered from the observed populations of small craters due to their rapid degradation. Impact-generated lunar regolith records the contribution from historical impacts of various sizes and is particularly sensitive to sub-hectometer craters, providing a unique means to estimate the small impactor flux. Here we estimate the distribution of regolith thickness in the Chang'E-5 landing region (the youngest radiometric-dated homogeneous mare unit) through both statistics of fresh crater morphology and regolith evolution simulations using different impact flux hypotheses. The large median regolith thickness of 3.6±0.3 m derived from crater morphology can be attributed solely to a higher production rate of small lunar craters at sub-hectometer scales, which is 1.2-1.6 times higher than previously estimated. Such an increased small impactor flux may occur at ∼600 Ma and indicate recent asteroid breakup events, or could have persisted over the past 2 Ga, as a result of the preferential delivery of small impactors through the Yarkovsky and YORP effects.

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月球嫦娥五号表层土撞击体通量撞击坑

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