Correlated compositional and mineralogical investigations at the Chang′e-3 landing site

Ling, Zongcheng; Jolliff, Bradley L.; Wang, Alian; Li, Chunlai; Liu, Jianzhong; Zhang, Jiang; Li, Bo; Sun, Lingzhi; Chen, Jian; Xiao, Long; Liu, Jianjun; Ren, Xin; Peng, Wen-Xi; Wang, Huan‐Yu; Cui, X. Z.; He, Zhiping; Wang, Yunlong

doi:10.1038/ncomms9880

Cited by 96 publications

(44 citation statements)

References 50 publications

(109 reference statements)

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“…Spectral data show HCP signatures associated with the mare unit, which is consistent with most lunar mare (e.g., Staid et al, ). However, in contrast to the CE‐3 landing site, olivine has not yet been detected at Von Kármán (Ling et al, ; Zhang et al, ), which suggests that the farside mare might be of slightly different composition. The mare unit is homogeneous and likely to represent a single eruptive episode during the lunar peak volcanic period that occurred in the Late Imbrian (3.80–3.20 Ga; e.g., Yingst & Head, ).…”

Section: Discussionmentioning

confidence: 99%

Geological Characteristics of Von Kármán Crater, Northwestern South Pole‐Aitken Basin: Chang'E‐4 Landing Site Region

et al. 2018

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Von Kármán crater (diameter = ~186 km), lying in the northwestern South Pole‐Aitken (SPA) basin, was formed in the pre‐Nectarian. The Von Kármán crater floor was subsequently flooded with one or several generations of mare basalts during the Imbrian period. Numerous subsequent impact craters in the surrounding region delivered ejecta to the floor, together forming a rich sample of the SPA basin and farside geologic history. We studied in details the targeted landing region (45.0–46.0°S, 176.4–178.8°E) of the 2018 Chinese lunar mission Chang'E‐4, within the Von Kármán crater. The topography of the landing region is generally flat at a baseline of ~60 m. Secondary craters and ejecta materials have covered most of the mare unit and can be traced back to at least four source craters (Finsen, Von Kármán L, Von Kármán L', and Antoniadi) based on preferential spatial orientations and crosscutting relationships. Extensive sinuous ridges and troughs are identified spatially related to Ba Jie crater (diameter = ~4 km). Reflectance spectral variations due to difference in both composition and physical properties are observed among the ejecta from various‐sized craters on the mare unit. The composition trends were used together with crater scaling relationships and estimates of regolith thickness to reconstruct the subsurface stratigraphy. The results reveal a complex geological history of the landing region and set the framework for the in situ measurements of the CE‐4 mission, which will provide unique insights into the compositions of farside mare basalt, SPA compositional zone including SPA compositional anomaly and Mg‐pyroxene annulus, regolith evolution, and the lunar space environment.

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Section: Discussionmentioning

confidence: 99%

Geological Characteristics of Von Kármán Crater, Northwestern South Pole‐Aitken Basin: Chang'E‐4 Landing Site Region

et al. 2018

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“…China's first lunar sample return mission, Chang'E‐5 (CE5) mission, is scheduled to launch in 2019, following the successful Chang'E‐3 (CE3) soft landing and roving exploration of northern Mare Imbrium (44.12°N, 19.51°W; Ling et al, ; Xiao, ; Xiao et al, ; Zou et al, ). The Rümker region in northern Oceanus Procellarum (41–45°N, 49–69°W, ~58,000 km 2 in area) is the landing region selected for the CE5 mission (Zeng et al, ).…”

Section: Introductionmentioning

confidence: 99%

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

et al. 2018

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The Rümker region (41–45°N, 49–69°W) is located in northern Oceanus Procellarum of the Moon. Mons Rümker is the most distinctive geological feature in the area. The region is characterized by prolonged lunar volcanism (Late Imbrian Period to Eratosthenian Period), forming multiple geologic units in the area, including very low‐Ti to low‐Ti mare basalts, high‐Ti mare basalts, and volcanic complexes. Each geologic unit has distinct element composition and mineral assemblages. The Rümker region, overlying the Procellarum KREEP Terrain, was selected as the landing region for China's Chang'E‐5 lunar sample return mission. Prelanding analyses of the geologic context and scientific potential are reported in this contribution. We conducted detailed geological mapping using image, spectral, and altimetry data. Fourteen geological units were defined, a geologic map was constructed, and the geologic history was outlined. The western mare units (Im1, Im2, and Im3) are Imbrian‐aged (~3.4–3.5 Ga) representing the major stage of lunar mare eruptive volcanism. The eastern young mare units (Em3 and Em4; <2 Ga) are among the youngest mare basalts on the Moon. They have never been explored in situ or studied in the laboratory. We suggest that samples returned from the eastern mare unit (Em4) could answer many fundamental questions and that this unit should be listed as the top priority landing site for Chang'E‐5 sample return mission.

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“…Our result, falling in the Apollo's range, is somewhat less than Apollo's upper limit, which is mainly attributed to the fact that, on one hand, the lunar dust was directly generated as a result of long‐term space weathering on the lunar surface, taking place continuously once it formed (Tang et al, ). The CE‐3 landing site is on the continuous ejecta deposits of a fresh impact crater (named Zi Wei) formed ~27 to ~100 million years ago (Fa et al, ; Ling et al, ; Xiao et al, ), which is younger than the Apollo 12 landing site (the Apollo 12 landing site was on the northwest rim of a 200‐m‐diameter impact crater formed 240 million years ago; Funkhouser, ), and thus, the CE‐3 landing site was much less weathered in contrast to Apollo 12 landing site. As a result, fewer lunar dust particles were formed in CE‐3 landing site due to the less space weathering time relative to Apollo 12, and thus, a low annual deposition rate was obtained in CE‐3 landing site.…”

Section: In Situ Measurement Results and Discussionmentioning

confidence: 99%

In Situ Measurements of Lunar Dust at the Chang'E‐3 Landing Site in the Northern Mare Imbrium

et al. 2019

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Lunar dust is regarded as the most crucial environmental problem on the Moon, and related research has crucially important scientific and technological interests. Here, we first reported the in situ measurements of lunar dust at the Chang'E‐3 landing site in the northern Mare Imbrium using temperature‐controlled sticky quartz crystal microbalance. The results showed that a total deposition mass at a height of 190 cm above the lunar surface during 12 lunar daytimes in the northern Mare Imbrium was about 0.0065 mg/cm2, corresponding to an annual deposition rate of ~21.4 μg/cm2, which is comparable with that of Apollo's result to some extent. The present researches are strategically important for future human and robotic lunar expeditions, and can provide a valuable reference for the design of dust protection for onboard payloads long‐term exposure to the lunar environment.

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Correlated compositional and mineralogical investigations at the Chang′e-3 landing site

Cited by 96 publications

References 50 publications

Geological Characteristics of Von Kármán Crater, Northwestern South Pole‐Aitken Basin: Chang'E‐4 Landing Site Region

Geological Characteristics of Von Kármán Crater, Northwestern South Pole‐Aitken Basin: Chang'E‐4 Landing Site Region

Geology and Scientific Significance of the Rümker Region in Northern Oceanus Procellarum: China's Chang'E‐5 Landing Region

In Situ Measurements of Lunar Dust at the Chang'E‐3 Landing Site in the Northern Mare Imbrium

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