Mineralogy, petrology, and chemistry of a Luna 16 basaltic fragment, sample B-1

Albee, A. L.; Chodos, A. A.; Gancarz, A. J.; Haines, E. L.; Papanastassiou, D. A.; Ray, L.; Tera, F.; Wasserburg, G. J.; Wen, Tao

doi:10.1016/0012-821x(72)90110-0

Cited by 38 publications

(24 citation statements)

References 11 publications

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“…The U datum reported in Albee et al (1972) obviously replicated (derived from the same work as) one of three disparate analyses reported in Tera and Wasserburg (1972a). (Fig.…”

Section: Documented-location Samples and The Latest Calibrationsupporting

confidence: 62%

“New” lunar meteorites: Implications for composition of the global lunar surface, lunar crust, and the bulk Moon

Warren

2005

Meteorit & Planetary Scien

144

139

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“…The U datum reported in Albee et al (1972) obviously replicated (derived from the same work as) one of three disparate analyses reported in Tera and Wasserburg (1972a). (Fig.…”

Section: Documented-location Samples and The Latest Calibrationsupporting

confidence: 62%

“New” lunar meteorites: Implications for composition of the global lunar surface, lunar crust, and the bulk Moon

Warren

2005

Meteorit & Planetary Scien

144

139

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“…3). Because solar Ar is released from the surface of grains at relatively low temperature, the medium to high (Albee et al, 1972;Grieve et al, 1972;Hollister and Kulick, 1972;Steele and Smith, 1972) and Luna 24 (Ryder et al, 1977;Vaniman and Papike, 1977;Coish and Taylor, 1978;Taylor et al, 1991;Papike et al, 1998;Papike and Vaniman, 1978 40 Ar values and errors are obtained from least squares fitting using the method of Williamson (1968). These fits also yield trapped 36 Ar t / 40 Ar compositions which are used to correct apparent ages which are shown in the form of age spectra, and the error on the trapped Ar ratio has been propagated through the age equation.…”

Section: Argon Mixing Diagram For the Lunar Regolith And Methods Of Agmentioning

confidence: 99%

Volcanism in Mare Fecunditatis and Mare Crisium: Ar-Ar age studies

Fernandes

Burgess

2005

Geochimica et Cosmochimica Acta

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“…The high‐alumina (HA) mare basalts are a unique group of mare basalts among the variety of rock types returned by the Apollo and Soviet Luna missions [e.g., Albee et al , 1972; Grieve et al , 1972; Helmke and Haskin , 1972; Ridley , 1975; Kurat et al , 1976; Ma et al , 1979; Shervais et al , 1985; Dickinson et al , 1985; Neal et al , 1988]. Their chemistry has implications for the nature of the mantle source from which they were derived and the evolution of the Lunar Magma Ocean [e.g., Taylor and Jakes , 1974; Snyder et al , 1992; Shearer and Papike , 1999].…”

Section: Introductionmentioning

confidence: 99%

Distinguishing high‐alumina mare basalts using Clementine UVVIS and Lunar Prospector GRS data: Mare Moscoviense and Mare Nectaris

Kramer¹,

Jolliff²,

Neal³

2008

J. Geophys. Res.

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[1] High-alumina (HA) mare basalts are a unique group of the lunar sample collection. Sample geochemistry indicates that these basalts are derived from sources composed of late-stage cumulates from the Lunar Magma Ocean (LMO). Their aluminous nature suggests their sources contained significant plagioclase, which has implications regarding the efficiency of plagioclase separation from earlier forming, mafic cumulates in the LMO to form the anorthositic lunar crust, and hence the heterogeneity of the lunar mantle. The Apollo and Luna missions sampled HA basalts from four different locations that are separated by 80 equatorial degrees ($2400 km). Radiometric age dating of these samples demonstrates aluminous basaltic volcanism spanned over 1 billion years, suggesting HA basalts may be more prevalent on the Moon than implied by the sample population. Knowing their global occurrence would ultimately enhance our understanding of lunar evolution. Aluminous mare basalts occupy a unique location in Th-FeO compositional space that suggests they can be identified using global remote-sensing data of the Moon. We present our approach for distinguishing exposures of HA basalts using Clementine ultraviolet-visible-infrared (UVVIS) and Lunar Prospector Gamma Ray Spectrometer (LP-GRS) data with constraints based on the FeO, TiO 2 , and Th abundances of Apollo and Luna HA samples. We identified 34 regions of interest (ROIs) where HA basalts could be a prominent component of the lunar surface. By analyzing the rims and proximal ejecta from small impacts (0.4-4 km in diameter) into the mare surface we characterized compositionally distinct basaltic units that make up the mare and thus determined which units represent HA basalt lavas. The results were used to generate maps that depict discrete mare units and classify their general basalt type. Here we focus on two ROIs: Mare Moscoviense and Mare Nectaris. Mare Moscoviense is composed of four basaltic units, two of which are HA candidates. Clementine UVVIS data of Mare Nectaris show evidence of up to three mare basalt units. One is the remnants of a mid-Ti unit that capped earlier low-Ti flows. The majority of the basin is filled by a compositionally indistinguishable low-Fe, low-Ti basalt. However, spectral profiles suggest there are two units. Regardless, the units both fit the criteria for a HA basalt.

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Mineralogy, petrology, and chemistry of a Luna 16 basaltic fragment, sample B-1

Cited by 38 publications

References 11 publications

“New” lunar meteorites: Implications for composition of the global lunar surface, lunar crust, and the bulk Moon

“New” lunar meteorites: Implications for composition of the global lunar surface, lunar crust, and the bulk Moon

Volcanism in Mare Fecunditatis and Mare Crisium: Ar-Ar age studies

Distinguishing high‐alumina mare basalts using Clementine UVVIS and Lunar Prospector GRS data: Mare Moscoviense and Mare Nectaris

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