Impact melt breccia and surrounding regolith measured by Chang'e-4 rover

Gou, Sheng; Yue, Zongyu; Di, Kaichang; Wang, Jia; Wan, Wenhui; Liu, Zhaoqin; Liu, Bin; Peng, Man; He, Zhiping; Xu, Rui

doi:10.1016/j.epsl.2020.116378

Cited by 14 publications

(20 citation statements)

References 38 publications

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“…Thus, the heterogeneity on the Moon can be well retained and is much stronger than that on the Earth. The remote-sensing spectrum and radar detection results show that there is a thick regolith layer on the top of the Von Kármán crater [1][2][3]. This provides an excellent opportunity for detection of the structural characteristics and the stacking mode of the lunar regolith, which are critical for understanding the formation process of the lunar regolith.…”

Section: Introductionmentioning

confidence: 99%

Self-Organization Characteristics of Lunar Regolith Inferred by Yutu-2 Lunar Penetrating Radar

Zhang

et al. 2021

Remote Sensing

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Most previous studies tend to simplify the lunar regolith as a homogeneous medium. However, the lunar regolith is not completely homogeneous, because there are weak reflections from the lunar regolith layer. In this study, we examined the weak heterogeneity of the lunar regolith layer using a self-organization model by matching the reflection pattern of both the lunar regolith layer and the top of the ejecta layer. After a series of numerical experiments, synthetic results show great consistency with the observed Chang’E-4 lunar penetrating radar data and provide some constraints on the range of controlling parameters of the exponential self-organization model. The root mean square permittivity perturbation is estimated to be about 3% and the correlation distance is about 5–10 cm. Additionally, the upper layer of ejecta has about 1–2 rocks per square meter, and the rock diameter is about 20–30 cm. These parameters are helpful for further study of structural characteristics and the evolution process of the lunar regolith. The relatively small correlation distance and root mean square perturbation in the regolith indicate that the regolith is mature. The weak reflections within the regolith are more likely to be due to structural changes rather than material composition changes.

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Section: Introductionmentioning

confidence: 99%

Self-Organization Characteristics of Lunar Regolith Inferred by Yutu-2 Lunar Penetrating Radar

Zhang

et al. 2021

Remote Sensing

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“…Based on the unique in situ spectral data obtained by VNIS, we have gained more information about the origin and evolution of the moon and space weathering [1,31,[41][42][43][44][45][46][47][48][49][50][51][52][53]. Li et al further analyzed the REFF spectra collected by VNIS on the first lunar day.…”

Section: Application Results Of Vnis On Board Chang'e-4mentioning

confidence: 99%

Applications of AOTF Spectrometers in In Situ Lunar Measurements

Gui

et al. 2021

Materials

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Spectrometers based on acousto-optic tunable filters (AOTFs) have several advantages, such as stable temperature adaptability, no moving parts, and wavelength selection through electrical modulation, compared with the traditional grating and Fourier transform spectrometers. Therefore, AOTF spectrometers can realize stable in situ measurement on the lunar surface under wide temperature ranges and low light environments. AOTF imaging spectrometers were first employed for in situ measurement of the lunar surface in the Chinese Chang’e project. The visible and near-infrared imaging spectrometer and the lunar mineralogical spectrometer have been successfully deployed on board the Chang’e-3/4 and Chang’e-5 missions. In this review, we investigate the performance indicators, structural design, selected AOTF performance parameters, data acquisition of the three lunar in situ spectral instruments used in the Chang’e missions. In addition, we also show the scientific achievement of lunar technology based on in situ spectral data.

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“…Along the rover path, small fresh craters featuring high‐reflectance materials on crater floors have been noticed (Figure ). There is no consensus yet about whether these small craters are primary (Lin et al., 2020) or secondary craters (Ding, Xiao, et al., 2020; Gou et al., 2020), but reflectance spectra revealed that the high‐reflectance materials were likely glass‐rich impact breccias (Gou et al., 2020; Lin et al., 2020). Melt‐bearing impact breccias returned by the Apollo missions have comparable relative permittivity with crystalline and igneous rocks (Chung et al., 1972), and topographic degradation of small craters on the Moon mainly occur as diffusive downslope movements on crater walls (Xie et al., 2017).…”

Section: Discussionmentioning

confidence: 99%