Characterization and interpretation of the global lunar impact basins based on remote sensing

Li, Jingwen; Liu, Jianzhong; Yue, Zongyu; Zhang, Li; Wang, Juntao; Zhu, K. J.

doi:10.1016/j.icarus.2022.114952

Cited by 10 publications

(10 citation statements)

References 51 publications

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“…Thus, 3.8 Ga should correspond to the Imbrian basalt and the age of the C-H basin should older than 3.9 Ga. This age range covers the result of Liu et al [24]. Considering the Stadius crater (Figure 17), which is located 186 km east of Copernicus, was obviously buried by Im2, the assumption that the C-H basin was buried by the Imbrian basalt, and the rim of the C-H basin is eroded by the ejecta from the Copernicus impact event and the weathering processes, is reasonable.…”

Section: Evolution Of the C-h Basinessupporting

confidence: 78%

“…Neumann et al measured the mascon as a buried peak-ring basin which is located at 7.2 • N 18.2 • W, with a rim diameter = 260 km and a peak-ring diameter = 130 km [16] (blue circle in Figure 3). The results of Liu et al confirm the basin type and the location of the central part of the basin, but they provide different values for the rim-to-rim diameter (483 km) and for the ring diameter (221 km) [24] (pink circle in Figure 3). Evans et al measured the mascon as a single ring basin, located at 7.28 • N 18.26 • W and 175 km in diameter (orange circles in Figure 3) [13].…”

Section: Morphology and Topographymentioning

confidence: 84%

“…The C-H basin's basic parameters are updated and located in 7. The C-H basin impact event occurred earlier than 3.9 Ga, maybe during the Aitkennian Epoch [24]. Then, a Hawaiian-style eruption formed the Sinus Aestuum-I DMD.…”

Section: Discussionmentioning

confidence: 99%

“…The Moon LRO LROC WAC Global Morphology Mosaic (100 m/pixel) and Moon LROC WAC DTM GLD100 In the south-eastern area of the Copernicus crater, a buried basin is present, called C-H [16]. The classification of the basin's type and the diameter is uncertain [13,16,20,24]. Such cases suggest that the current basin catalogs need further correction.…”

Section: Datasetsmentioning

confidence: 99%

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Study of the Buried Basin C-H, Based on the Multi-Source Remote Sensing Data

Zhang

et al. 2022

Remote Sensing

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We use multi-source remote sensing data to identify the details of a mascon south-east of the lunar Copernicus crater. Studies of the topography, gravity, geochronology and mineral are combined to prove that the mascon is a buried peak-ring basin with diameters of about 130 km and 260 km. The underground structure is covered by 890 m thick mare basalts, as determined by analyzing the spectral features of the impact crater, Copernicus H. The determination of the crater size–frequency distribution (CSFD) suggests that the impact that created the C-H basin occurred earlier than 3.9 Ga. Then, a Hawaiian-style eruption in the late Imbrian period formed the Sinus Aestuum-I dark mantling deposit (DMD). Soon, mare basalts covered the basin several times from 3.8 Ga. Finally, the ejecta from the Copernicus impact event at about 800 Ma, and the weathering processes caused the disappearance of the C-H basin rim from the lunar surface.

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Section: Evolution Of the C-h Basinessupporting

confidence: 78%

Section: Morphology and Topographymentioning

confidence: 84%

Section: Discussionmentioning

confidence: 99%

Section: Datasetsmentioning

confidence: 99%

See 2 more Smart Citations

Study of the Buried Basin C-H, Based on the Multi-Source Remote Sensing Data

Zhang

et al. 2022

Remote Sensing

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“…A buried basin to the south-eastern of Copernicus was given different diameter and classify as different types of basins [10,13,17]. Such case suggests that the current basin catalogs need further correction.…”

Section: Introductionmentioning

confidence: 99%

Study of Buried Basin in Copernicus Area Based on Multi Source Remote Sensing Data

Xu¹,

Zhang²,

Teng³

et al. 2022

Preprint

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Masons are often overlooked part of impact basins, but play an important role in revealing the lunar history. Previous study in masons were usually limited to gravity data. Few researches were reported on morphology features and chronology, which hampers the construction of a complete geological interpretation for the evolution of each mascons. We use multi source remote sensing data to identify the details characteristic of mascons. Result of topography, gravity and characteristic are combined to prove that a mason beside Copernicus crater is a buried peak-ring basin which is about 130km and 260km in diameter. The underground structure is of confirmed as 890m thick mare basalts by analyzing the spectral feature of the material in a geological outcrop called Copernicus H. Geology evolution analysis joint crater size-frequency distribution (CSDF) dating demonstrate that the buried basin impact event occurred in 3.6Ga. Then a hawaiian-style eruption in late Imbrian formed Sinus Aestuum Ⅰ Dark Mantling Deposit (DMD). Mare basalts filling in 3.4Ga. After that, ejecta from Copernicus impact event in about 820Ma and weathering processes cause the disappearing from lunar surface of the buried basin.

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