Mechanisms for incompatible-element enrichment on the Moon deduced from the lunar basaltic meteorite Northwest Africa 032

Borg, L. E.; Gaffney, Amy M.; Shearer, C. K.; DePaolo, Donald J.; Hutcheon, I. D.; Owens, T.L.; Ramon, E; Brennecka, G. A.

doi:10.1016/j.gca.2009.03.039

Cited by 78 publications

(109 citation statements)

References 45 publications

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“…However, the radiogenic ages of basaltic lunar meteorites extend the duration of mare volcanism to younger ages ≤3 Ga. Borg et al (2009) reported Nd-Sm crystallization ages of 2.993 ± 0.032 Ga for an olivine cumulate gabbro (OC) clast from the basaltic breccia Northwest Africa (NWA) 773 and 2.931 ± 0.092 Ga for mare basalt NWA 032; Wang et al (2012) gave a Pb-Pb crystallization age of 3.073 ± 0.015 Ga for Zr-rich minerals in mare basalt NWA 4734; Anand et al (2006) reported a U-Pb age of 2.929 ± 0.15 Ga for phosphates in mare basalt LaPaz Icefield (LAP) 02205. These younger ages are consistent with the model ages based on crater counts from mare surfaces (Hiesinger and Head 2006).…”

Section: Introductionmentioning

confidence: 99%

“…The pairing of NWA 2977 with NWA 773 is supported further by similar isotopic ages that are relatively young for lunar rocks. The radiogenic isotope data from the NWA 773 OC include a 147 Sm/ 143 Nd age of 2.993 ± 0.032 Ga (Borg et al 2009), an 40 Ar-39 Ar step-heating age of approximately 2.91 Ga (Fernandes et al 2003), and 207 Pb analyses of baddeleyite crystals indicating an age of 3.131 ± 0.012 Ga (Shaulis et al 2013). The radiogenic ages of NWA 2977 include whole-rock ages of 2.77 ± 0.04 Ga for Ar-Ar (Burgess et al 2007), 3.10 ± 0.05 Ga for Nd-Sm, 3.29 ± 0.11 Ga for Rb-Sr (Nyquist et al 2009), and 3.12 ± 0.01 Ga for Pb-Pb baddeleyite (Zhang et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Breccias of the NWA 773 clan contain a variety of mafic clasts, including the OC (Bunch et al 2006). The OC lithology has one of the youngest crystallization ages among lunar samples collected (e.g., Borg et al 2009;Nyquist et al 2009;Zhang et al 2011). Many of the breccia clasts are considered to be parts of a comagmatic crystallization sequence, with the OC representing an early stage of magmatic differentiation (Fagan et al 2003(Fagan et al , 2014Jolliff et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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Mineralogy and petrology of lunar meteorite Northwest Africa 2977 consisting of olivine cumulate gabbro including inverted pigeonite

et al. 2015

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Lunar meteorite Northwest Africa (NWA) 2977 is identified as an olivine cumulate gabbro (OC), consisting of coarse cumulate olivine crystals up to 1 mm with low-Ca and high-Ca pyroxenes, plagioclase, and interstitial incompatible element-rich pockets of K-feldspar, Ca-phosphates, ilmenite, and troilite. These minerals and textures are similar to those of the OC clasts of the NWA 773 clan of meteorites. NWA 2977 contains a variety of pyroxene textures and compositions including augite, pigeonite, and rare orthopyroxene, all having exsolution lamellae. Some of the orthopyroxene has abundant augite lamellae with compositions indicating formation by inversion of pigeonite. This pigeonite was inverted at 1140°C according to the pigeonite eutectoid reaction (PER) temperatures. Inverted pigeonite has not been found previously in the NWA 773 clan of meteorites. The presence of inverted pigeonite indicates that NWA 2977 cooled more slowly than most other OC clasts of the NWA 773 clan. The relatively slow cooling of NWA 2977 can be explained by formation in a deeper level of the original igneous body of the NWA 773 clan OC lithology.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mineralogy and petrology of lunar meteorite Northwest Africa 2977 consisting of olivine cumulate gabbro including inverted pigeonite

et al. 2015

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“…Ages of lunar crustal rocks characterized by high proportions of anorthitic feldspar, and thus interpreted as representing primary lunar crust, range from 4.57 to 4.36 Ga ( [87,88] for a review see [55]) while models of solidification range from 10 to 200 Myrs depending on whether tidal eating is invoked ( [69,89] respectively). Ages associated with formation of the KREEP reservoir range from 4.48 Ga (from Apollo 14 zircons) [90] to 4.36 Ga (Lu-Hf isotopic systematics on KREEP basalts) [91].…”

Section: The Lunar Magma Oceanmentioning

confidence: 99%

Sources of Extraterrestrial Rare Earth Elements: To the Moon and Beyond

McLeod

Krekeler

2017

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Abstract:The resource budget of Earth is limited. Rare-earth elements (REEs) are used across the world by society on a daily basis yet several of these elements have <2500 years of reserves left, based on current demand, mining operations, and technologies. With an increasing population, exploration of potential extraterrestrial REE resources is inevitable, with the Earth's Moon being a logical first target. Following lunar differentiation at~4.50-4.45 Ga, a late-stage (after~99% solidification) residual liquid enriched in Potassium (K), Rare-earth elements (REE), and Phosphorus (P), (or "KREEP") formed. Today, the KREEP-rich region underlies the Oceanus Procellarum and Imbrium Basin region on the lunar near-side (the Procellarum KREEP Terrain, PKT) and has been tentatively estimated at preserving 2.2 × 10 8 km 3 of KREEP-rich lithologies. The majority of lunar samples (Apollo, Luna, or meteoritic samples) contain REE-bearing minerals as trace phases, e.g., apatite and/or merrillite, with merrillite potentially contributing up to 3% of the PKT. Other lunar REE-bearing lunar phases include monazite, yittrobetafite (up to 94,500 ppm yttrium), and tranquillityite (up to 4.6 wt % yttrium, up to 0.25 wt % neodymium), however, lunar sample REE abundances are low compared to terrestrial ores. At present, there is no geological, mineralogical, or chemical evidence to support REEs being present on the Moon in concentrations that would permit their classification as ores. However, the PKT region has not yet been mapped at high resolution, and certainly has the potential to yield higher REE concentrations at local scales (<10s of kms). Future lunar exploration and mapping efforts may therefore reveal new REE deposits. Beyond the Moon, Mars and other extraterrestrial materials are host to REEs in apatite, chevkinite-perrierite, merrillite, whitlockite, and xenotime. These phases are relatively minor components of the meteorites studied to date, constituting <0.6% of the total sample. Nonetheless, they dominate a samples REE budget with their abundances typically 1-2 orders of magnitude enriched relative to their host rock. As with the Moon, though phases which host REEs have been identified, no extraterrestrial REE resource, or ore, has been identified yet. At present extraterrestrial materials are therefore not suitable REE-mining targets. However, they are host to other resources that will likely be fundamental to the future of space exploration and support the development of in situ resource utilization, for example: metals (Fe, Al, Mg, PGEs) and water.

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“…On the nearside of the Moon, global remote sensing observations by gamma-ray spectrometers [e.g., 13,14] verified the enrichment of K, Th, U in/around Oceanus Procellarum and Mare Imbrium (called as Procellarum KREEP Terrene, PKT) [15]. Rocks with KREEP-like compositions may have been associated with residue of the lunar magma ocean (urKREEP) located between anorthositic crust and mantle [16], however, some KREEP-like rocks might have been affected by low degrees of partial melting or other processes that would lead to enrichments in incompatible elements [17]. In the former case, KREEP-rich rocks provide a link to the late-stage-magma composition in lunar magma ocean.…”

Section: Th-rich Regions In Procellarum Kreep Terranementioning

confidence: 99%

Instrumental Overview of an Active X-ray Spectrometer for Future Lunar Landing Mission

Nagaoka

Hasebe

Kusano

et al. 2016

Proceedings of International Symposium on Radiation Detectors and Their Uses (ISRD2016)

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An Active X-ray Spectrometer (AXS) is being developed as a rover-based elemental analyzing device for future lunar and planetary missions in order to obtain in situ geochemical analyses of rocks, regolith, and soil near landing sites. The AXS is composed of four active X-ray generators with pyroelectric crystals and a silicon drift detector (SDD). In this paper, the instrumental overview of AXS for future lunar and planetary landing/sample-return missions, and possible scientific targets of a lunar landing mission are presented and discussed.

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Mechanisms for incompatible-element enrichment on the Moon deduced from the lunar basaltic meteorite Northwest Africa 032

Cited by 78 publications

References 45 publications

Mineralogy and petrology of lunar meteorite Northwest Africa 2977 consisting of olivine cumulate gabbro including inverted pigeonite

Mineralogy and petrology of lunar meteorite Northwest Africa 2977 consisting of olivine cumulate gabbro including inverted pigeonite

Sources of Extraterrestrial Rare Earth Elements: To the Moon and Beyond

Instrumental Overview of an Active X-ray Spectrometer for Future Lunar Landing Mission

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