MTE Features of Apollo Basin and Its Significance in Understanding the SPA Basin

Meng, Zhiguo; Wang, Yongzhi; Chen, Shengbo; Zheng, Yongchun; Shi, Jiancheng; Wang, Tianxing; Zhang, Yuanzhi; Ping, Jinsong; Hou, Lele

doi:10.1109/jstars.2019.2916061

Cited by 10 publications

(43 citation statements)

References 36 publications

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“…The CELMS data processing procedure is similar to that of the processing used in Mare Imbrium and Apollo Basin [17,18]. Firstly, the time angle, defined as the longitude difference between the observation point and the subsolar point, is used to attribute the selected data into 24 time spans.…”

Section: T B Maps Generationmentioning

confidence: 99%

“…These time spans represent the two extreme phases of the MTE, which are appropriate to study the regolith thermophysical features of the basaltic units [17,18,32]. spans represent the two extreme phases of the MTE, which are appropriate to study the regolith thermophysical features of the basaltic units [17,18,32]. spans represent the two extreme phases of the MTE, which are appropriate to study the regolith thermophysical features of the basaltic units [17,18,32].…”

Section: T B Maps Generationmentioning

confidence: 99%

“…35 GHz, and 8.1 cm to 16.2 cm at 37 GHz, which is decided by the FTA of the lunar regolith [15][16][17][18]. Moreover, the CELMS data has been proved to be sensitive to the substrate compositions and temperature [16][17][18]20,21]. Therefore, the CELMS data provides a potential chance to better understand the basaltic units in Mare Moscoviense.…”

Section: Introductionmentioning

confidence: 99%

“…The different understanding of the basaltic units also presents the difficulty in studying the basaltic volcanism by only using the spectral data. This is mainly because the penetration depth of the used spectral data is rather low, only several microns below the lunar regolith [15][16][17][18]. In such depth, the regolith can easily be affected by the space weathering and the impact ejecta from nearby, or even far away regions [14,15].…”

Section: Introductionmentioning

confidence: 99%

“…How to mitigate such disadvantages and to better explore the regolith thermophysical features in situ is a critical problem in current lunar studies. It is known that the observations in the microwave domain can eliminate well the aforementioned disadvantages [15][16][17][18]. For the first time, the Microwave Sounder (CELMS) onboard Chang'E-1/2 (CE-1/2) missions was used to measure the thermal emission of the lunar regolith in microwave domain.…”

Section: Introductionmentioning

confidence: 99%

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Reevaluating Mare Moscoviense And Its Vicinity Using Chang’e-2 Microwave Sounder Data

et al. 2020

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Mare Moscoviense (148°E, 27°N) is one of the few large maria on the lunar farside, with the thinnest crust and a positive gravity anomaly. In this paper, the Chang’E-2 Microwave Sounder (CELMS) data was employed to study the microwave thermal emission features of mare basalts in Moscoviense Basin. The time angle and linear interpolation method are used to generate the brightness temperature (TB) maps at noon and night, as well as the TB difference (dTB) map. The obtained important results are as follows. (1) A new geologic map is generated with the TB and dTB maps using the maximum likelihood method, which gives a new expression about the basaltic units in Mare Moscoviense compared to the optical results; (2) the substrate temperature of Moscoviense Basin is likely warmer than what we know; (3) unit Ihtm (a Late (?) Imbrian, mid- to high-Ti, high-Fe basalt) is re-understood as two independent volcanic features with their own fissures; (4) the dTB maps firstly indicate that the depth lunar regolith is homogeneous in the highlands surrounding Mare Moscoviense, at least in the microwave domain, and secondly that there exists a special material bringing about the low dTB anomaly in the shallow layer of the east highlands. The results will be of great significance to better understand the basaltic volcanism of the Moon.

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Section: T B Maps Generationmentioning

confidence: 99%

Section: T B Maps Generationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Reevaluating Mare Moscoviense And Its Vicinity Using Chang’e-2 Microwave Sounder Data

et al. 2020

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Mare Deposits Identification and Feature Analysis in Mare Australe Based on CE‐2 CELMS Data

et al. 2020

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The microwave signal has the penetration capability, which provides a potential chance to improve understanding of the mare deposits and the formation process of Mare Australe, a complex, extensive, and poorly understood region on the Moon. In this paper, the Chang'E‐2 microwave radiometer (CELMS) data were selected and processed to evaluate the microwave thermal emission features of the mare deposits in Mare Australe. After comparison, the dTB map at 3.0 GHz is employed. The results are as follows. (a) The possible cryptomare is much more extensive in Australe region than that identified with optical data. (b) The basaltic volcanism is re‐understood as three major episodes. (c) The high dTB anomaly is interpreted as the location of the vent areas in the mare patches. (d) The K‐means algorithm was first used to process the CELMS data, and the identified linear and ring structures indicate some important information about the formation processes of Mare Australe. These special findings will be of fundamental significance to better understand the basaltic volcanism and the evolution of the lunar surface.

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Geological Background of the Chang'e 6 Landing Site and the Provenance of Returned Samples

Gao,

Xiao,

Wueller

et al. 2024

JGR Planets

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China's Chang'e‐6 (CE‐6) is the first mission in human history to return samples from the far side of the Moon. CE‐6 landed in the mare plains of the southern Apollo basin (153.98°W, 41.63°S) within the South Pole‐Aitken (SPA) basin on 2 June 2024 and returned 1,935.3 g of samples on 25 June 2024. The unique geological history of the Apollo basin offers an opportunity to address several important scientific questions in lunar science. To provide geological context for the analysis of the returned samples, we described the geology of the area surrounding the CE‐6 landing site in detail. We interpreted that the region exhibits three periods of mare basaltic volcanism (EmSAp1, EmSAp2 and EmSAp3) separated by one billion years. CE‐6 landed on the EmSAp2 unit, with a model age of ∼2.8 Ga. Several post‐mare impacts occurring outside this region also contributed foreign materials to CE‐6 landing site. We anticipate that the returned samples are dominated by local EmSAp2 materials, and may also include younger high‐Ti basalt from the EmSAp3 unit, older low‐Ti basalt from the EmSAp1 unit, ejecta from younger craters such as Chaffee S and O’Day, and ejecta from craters outside the SPA basin such as Vavilov, Crookes, and Das. The estimated total feldspathic exotic ejecta in the regolith of CE‐6 sample zone is 30%. Our study indicates that the regolith in the CE‐6 sampling area is rich in scientific value for understanding lunar volcanism and impact history and offers the possibility of further calibrating the lunar cratering chronology.

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MTE Features of Apollo Basin and Its Significance in Understanding the SPA Basin

Cited by 10 publications

References 36 publications

Reevaluating Mare Moscoviense And Its Vicinity Using Chang’e-2 Microwave Sounder Data

Reevaluating Mare Moscoviense And Its Vicinity Using Chang’e-2 Microwave Sounder Data

Mare Deposits Identification and Feature Analysis in Mare Australe Based on CE‐2 CELMS Data

Geological Background of the Chang'e 6 Landing Site and the Provenance of Returned Samples

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