A summary of relative ages of lunar nearside and farside plains

Boyce, J. M.; Dial, A. L.; Soderblom, Laurence A.

doi:10.3133/ofr75141

Cited by 6 publications

(5 citation statements)

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“…Areally small geologic units often cannot be dated accurately by counts of craters because too few have formed after the units were deposited. The technique is based on a model for crater erosion developed by Soderblom and Lebofsky (1972) and refined and applied by Boyce (1976;Soderblom and Boyce, 1972;Boyce et al, 1974;. The method is a quantitative descendant of a system for dating small craters devised by Trask (1969Trask ( , 1971 which was successfully applied to mare surfaces being considered for Apollo landings (fig.…”

Section: Crater Morphologymentioning

confidence: 99%

“…Courtesy E. A. Whitaker (1972). (1973,1975); Boyce et al (1974Boyce et al ( , 1975; Boyce (1976); ). 3.…”

Section: Remote Sensingmentioning

confidence: 99%

“…Table 6.7 and the geologic and paleogeologic maps (color plates C and D) give some indication of the relations between age and spectral type of mare units (Boyce et al, 1974;Head et al, 1978a, b;Whitford-Stark and Head, 1980;Pieters et al, 1980;BVSP, 1981, ch. 2).…”

Section: Stratigraphy and Distributionmentioning

confidence: 99%

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The geology of the terrestrial planets

Carr¹

1983

Reviews of Geophysics

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During the last four years our knowledge of the geology of the terrestrial planets has advanced rapidly. The advances are particularly noticeable for Venus and Mars. Improved understanding of Venus has come largely from the Pioneer Venus mission (Colin, 1980), which has given us our first global view of the planet, albeit at fairly low resolution. The period was also one of almost continuous data gathering for Mars as the Viking orbiters and landers, emplaced at the planet in 1976, continued to function.

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Section: Crater Morphologymentioning

confidence: 99%

“…Courtesy E. A. Whitaker (1972). (1973,1975); Boyce et al (1974Boyce et al ( , 1975; Boyce (1976); ). 3.…”

Section: Remote Sensingmentioning

confidence: 99%

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The geology of the terrestrial planets

Carr¹

1983

Reviews of Geophysics

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“…9; Soderblom and Boyce, 1972;Boyce and Dial, 1974;Boyce and others, 1974). More recent work (Boyce and Dial, 1975;Boyce, 1976 (Shoemaker, 1970;Soderblom and Lebofsky, 1972;Soderblom and Boyce, 1972;Boyce, 1975).…”

Section: Relative Ages Of Lunar Plainsmentioning

confidence: 97%

Lunar remote sensing and measurements

Moore¹,

Boyce²,

Schaber³

et al. 1980

Professional Paper

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“…Previous research has included extensive remote sensing dating work on mare basalts in the Oceanus Procellarum region. Boyce et al (1974) [42] and Boyce (1976) [43] used crater morphology methods to establish a model age of 2.5 Ga for Oceanus Procellarum, considering Aristarchus as the youngest area, with a model age of 1.7 Ga. Young (1977) [44] conducted CSFD measurements in the northern part of Oceanus Procellarum, suggesting that lunar mare volcanic activity may have persisted until ~1.97 Ga to ~1.57 Ga. Schultz and Spudis (1983) [45] proposed that basalts surrounding the Lichtenberg crater in the middle of Oceanus Procellarum are younger than 1 Ga. Hiesinger et al (1998;2002; [5,18,19,25,[46][47][48] classified mare basalt units using Clementine data and determined mare basalt ages through CSFD measurements. In the Oceanus Procellarum region, mare basalts have been determined to have ages ranging from ~3.7 Ga to ~1.2 Ga, with the youngest mare basalts located around the Aristarchus plateau, considering the Oceanus Procellarum and Mare Imbrium regions as the youngest areas [5].…”

Section: Introductionmentioning

confidence: 99%

Geomorphology, Mineralogy, and Chronology of Mare Basalts in the Oceanus Procellarum Region

Zhang,

Chen,

Pan

et al. 2024

Remote Sensing

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Mare basalts on the lunar surface are tangible expressions of the complex thermal evolution and geological processes that have occurred within the lunar interior. These basaltic manifestations are highly important because they provide invaluable insights into lunar geological evolution. Notably, the Oceanus Procellarum region, which is renowned for its extensive and long-lasting basaltic volcanism, is a premier location to investigate late-stage lunar thermal evolution. The primary aim of this research is to elucidate the geomorphological, compositional, and temporal attributes that define the mare basalts within the Oceanus Procellarum region. To achieve this aim, we comprehensively analyzed the geomorphological features present within the region, leveraging Kaguya/SELENE TC images and digital elevation models. Specifically, these geomorphological features encompass impact craters, wrinkle ridges, sinuous rilles, and volcanic domes. Subsequently, we thoroughly examined the mineralogical attributes of basalts in the Oceanus Procellarum region, leveraging Kaguya/SELENE MI data and compositional map products. To more accurately reflect the actual ages of the mare basalts in the Oceanus Procellarum region, we carefully delineated the geological units within the area and employed the latest crater size-frequency distribution (CSFD) technique to precisely determine their ages. This refined approach allowed for a more comprehensive and accurate understanding of the basaltic rocks in the study area. Overall, our comprehensive study included an in-depth analysis of the volcanic activity and evolution of the Oceanus Procellarum region, along with an examination of the correlation between the mineralogical composition and ages of mare basalts. The findings from this exhaustive investigation reveal a definitive age range for basalt units within the Oceanus Procellarum region from approximately 3.69 Ga to 1.17 Ga. Moreover, the latest mare basalts that formed were pinpointed north of the Aristarchus crater. Significantly, the region has experienced at least five distinct volcanic events, occurring approximately 3.40 Ga, 2.92 Ga, 2.39 Ga, 2.07 Ga, and 1.43 Ga, leading to the formation of multiple basalt units characterized by their unique mineral compositions and elemental abundances. Through the application of remote sensing mineralogical analysis, three primary basalt types were identified: low-titanium, very-low-titanium, and intermediate-titanium basalt. Notably, the younger basalt units exhibit an elevated titanium proportion, indicative of progressive olivine enrichment. Consequently, these younger basalt units exhibit more intricate and complex mineral compositions, offering valuable insights into the dynamic geological processes shaping the lunar surface.

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A summary of relative ages of lunar nearside and farside plains

Cited by 6 publications

References 0 publications

The geology of the terrestrial planets

The geology of the terrestrial planets

Lunar remote sensing and measurements

Geomorphology, Mineralogy, and Chronology of Mare Basalts in the Oceanus Procellarum Region

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