The origin of young mare basalts inferred from lunar meteorites Northwest Africa 4734, 032, and LaPaz Icefield 02205

Elardo, S. M.; Shearer, C. K.; Fagan, A. L.; Borg, L. E.; Gaffney, Amy M.; Burger, P. V.; Neal, C. R.; Fernandes, V. A.; McCubbin, F. M.

doi:10.1111/maps.12239

Cited by 64 publications

(73 citation statements)

References 108 publications

(172 reference statements)

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“…Although RE-merrillite is more abundant than apatite, fewer RE-merrillite analyses exist in the literature, and little is known about the variation in RE-merrillite composition within the Mg-suite. Of the analyses that are available, Mg-suite RE-merrillite consistently has an elevated Mg#, ranging from 85 to 98 (Neal et al 1990;Neal and Taylor 1991;Jolliff et al 1993Jolliff et al , 2006Elardo et al 2012;McCallum and Mathez 1975), whereas RE-merrillite in mare basalts extend to much more Fe-rich compositions with a total Mg# ranging from 3 to 86 (Griffin et al 1972;Frondel 1975;Smith and Steele 1976;Neal and Taylor 1991;Zeigler et al 2005;Jolliff et al 2006;Elardo et al 2014). Additional efforts to characterize RE-merrillite in lunar samples and its relationship to apatite is a clear topic requiring further development.…”

Section: Phosphatesmentioning

confidence: 96%

“…Despite their KREEP-rich nature, Mg-suite rocks have apatite with REE abundances that are generally lower than REE abundances in apatites from mare basalts (Fig. 8;Jolliff et al 1993;McCubbin et al 2010bMcCubbin et al , 2011Tartèse et al 2013;Barnes et al 2014;Elardo et al 2014). On the surface, this observation seems counter-intuitive, but in many mare basalts apatite is the primary REE-hosting phase, whereas RE-merrillite is the primary REE-hosting phase in the Mg-suite rocks (McCubbin et al 2011).…”

Section: Phosphatesmentioning

confidence: 96%

“…The brecciated feldspathic lunar meteorite Dhofar 489 contains clasts of both magnesian anorthosite and spinel troctolite (Jolliff et al 1993;McCubbin et al 2010bMcCubbin et al , 2011Tartèse et al 2013Tartèse et al , 2014Barnes et al 2014;Elardo et al 2014). c.…”

Section: Dhofar 489: Magnesian Anorthosite and Spinel Troctolite Clastsmentioning

confidence: 99%

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Origin of the lunar highlands Mg-suite: An integrated petrology, geochemistry, chronology, and remote sensing perspective

Shearer

Elardo

Petro

et al. 2014

American Mineralogist

130

154

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The Mg-suite represents an enigmatic episode of lunar highlands magmatism that presumably represents the first stage of crustal building following primordial differentiation. This review examines the mineralogy, geochemistry, petrology, chronology, and the planetary-scale distribution of this suite of highlands plutonic rocks, presents models for their origin, examines petrogenetic relationships to other highlands rocks, and explores the link between this style of magmatism and early stages of lunar differentiation. Of the models considered for the origin of the parent magmas for the Mg-suite, the data best fit a process in which hot (solidus temperature at ≥2 GPa = 1600 to 1800 °C) and less dense (r ~3100 kg/m 3 ) early lunar magma ocean cumulates rise to the base of the crust during cumulate pile overturn. Some decompressional melting would occur, but placing a hot cumulate horizon adjacent to the plagioclase-rich primordial crust and KREEP-rich lithologies (at temperatures of <1300 °C) would result in the hybridization of these divergent primordial lithologies, producing Mg-suite parent magmas. As urKREEP (primeval KREEP) is not the "petrologic driver" of this style of magmatism, outside of the Procellarum KREEP Terrane (PKT), Mg-suite magmas are not required to have a KREEP signature. Evaluation of the chronology of this episode of highlands evolution indicates that Mg-suite magmatism was initiated soon after primordial differentiation (<10 m.y.). Alternatively, the thermal event associated with the mantle overturn may have disrupted the chronometers utilized to date the primordial crust. Petrogenetic relationships between the Mg-suite and other highlands suites (e.g., alkali-suite and magnesian anorthositic granulites) are consistent with both fractional crystallization processes and melting of distinctly different hybrid sources.

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Section: Phosphatesmentioning

confidence: 96%

Section: Phosphatesmentioning

confidence: 96%

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Origin of the lunar highlands Mg-suite: An integrated petrology, geochemistry, chronology, and remote sensing perspective

Shearer

Elardo

Petro

et al. 2014

American Mineralogist

130

154

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“…McCubbin et al (2011) used the apatites from mare basalts to determine the relative abundances of H 2 O, F, and Cl in the mare source regions using a relative volatile abundance diagram derived by experimental data on apatite-melt partitioning for F, Cl, and H 2 O, which was later refined by McCubbin et al (2013). We have updated this plot to include more recent mare basalt apatites from the literature (Elardo et al 2014;McCubbin et al 2010c; (Fig. 11b).…”

Section: Abundances Of F CL and H 2 O In Urkreepmentioning

confidence: 97%

“…Truncated ternary plots of apatite X-site occupancy (mol%) from mare basalts high-Al basalts, KREEP basalts, magnesian and alkali suite rocks, and impact melt rocks. Data yielding (F+Cl) > 1 atom are plotted along the OH -free join assuming 1 -Cl = F. Data used for plot are from literature (Boyce et al 2010;Elardo et al 2014;McCubbin et al 2011McCubbin et al , 2010bMcCubbin et al , 2010cTartèse et al 2014b;Taylor et al 2004) with the exception of apatite from high-Al basalt 14321,1842 where the EPMA data are available in a supplementary data table 1 available online. still suggested graphite was present at depth and the oxidation of this graphite is capable of producing the pyroclastic eruption of the lunar fire-fountains.…”

Section: Volatile-bearing Mineralogymentioning

confidence: 99%

Magmatic volatiles (H, C, N, F, S, Cl) in the lunar mantle, crust, and regolith: Abundances, distributions, processes, and reservoirs

McCubbin

Kaaden

Tartèse

et al. 2015

American Mineralogist

Self Cite

180

106

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Many studies exist on magmatic volatiles (H, C, N, F, S, Cl) in and on the Moon, within the last several years, that have cast into question the post-Apollo view of lunar formation, the distribution and sources of volatiles in the Earth-Moon system, and the thermal and magmatic evolution of the Moon. However, these recent observations are not the first data on lunar volatiles. When Apollo samples were first returned, substantial efforts were made to understand volatile elements, and a wealth of data regarding volatile elements exists in this older literature. In this review paper, we approach volatiles in and on the Moon using new and old data derived from lunar samples and remote sensing. From combining these data sets, we identified many points of convergence, although numerous questions remain unanswered.The abundances of volatiles in the bulk silicate Moon (BSM), lunar mantle, and urKREEP [last ~1% of the lunar magma ocean (LMO)] were estimated and placed within the context of the LMO model. The lunar mantle is likely heterogeneous with respect to volatiles, and the relative abundances of F, Cl, and H 2 O in the lunar mantle (H 2 O > F >> Cl) do not directly reflect those of BSM or urKREEP (Cl > H 2 O ≈ F). In fact, the abundances of volatiles in the cumulate lunar mantle were likely controlled by partitioning of volatiles between LMO liquid and nominally anhydrous minerals instead of residual liquid trapped in the cumulate pile. An internally consistent model for lunar volatiles in BSM should reproduce the absolute and relative abundances of volatiles in urKREEP, the anorthositic primary crust, and the lunar mantle within the context of processes that occurred during the thermal and magmatic evolution of the Moon. Using this mass-balance constraint, we conducted LMO crystallization calculations with a specific focus on the distributions and abundances of F, Cl, and H 2 O to determine whether or not estimates of F, Cl, and H 2 O in urKREEP are consistent with those of the lunar mantle, estimated independently from the analysis of volatiles in mare volcanic materials. Our estimate of volatiles in the bulk lunar mantle are 0.54-4.5 ppm F, 0.15-5.3 ppm H 2 O, 0.26-2.9 ppm Cl, 0.014-0.57 ppm C, and 78.9 ppm S. Our estimates of H 2 O are depleted compared to independent estimates of H 2

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New Insights Into Lithology Distribution Across the Moon

Wang

Zhao

2017

JGR Planets

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Lithology distribution across the Moon is pivotal for understanding lunar evolution. However, so far, the distribution of lunar rock suites is still uncertain; as a result, many related core issues on lunar evolution have long been in dispute. This work reports on a new lithology distribution map across the Moon and discusses some critical issues of the lunar evolutionary process. The oxide abundances derived from Chang'E‐1 Interference Imaging Spectrometer imagery and the Th contents inferred by Lunar Prospector Gamma Ray and Neutron Spectrometer data are employed to generate the lithological map by using the decision tree C5.0 algorithm. The following conclusions are inferred from this new map. (1) Magnesian suite is widely distributed across the Feldspathic Highlands Terrane and in the periphery of the South Pole‐Aitken Terrane. Thus, the viewpoints have been validated that the early magnesian magmatism may be a global phenomenon and that KREEP basalt is not necessary for the petrogenesis of Mg‐rich rocks. Moreover, the regions of Dryden, Chaffee S, Theophilus, and Moscoviense are confirmed as magnesian suite exposures. (2) The observation that the Feldspathic Highlands Terrane has a higher Mg/(Mg + Fe) value than the maria is related to the flood of the Mg suite across the Feldspathic Highlands Terrane. (3) The specific exposed locations of the alkali suite across the Moon have long been unsolved, and this work discloses that the alkali suite prevails in the outskirts of the Procellarum KREEP Terrane, the center of the South Pole‐Aitken Terrane, and some isolated locales. (4) Focusing on distinguishing mare basalts from other mafic rocks, seven geochemical indices are proposed to determine the potential exposures of mare basalts across the Moon. (5) In Mare Insularum, a series of KREEP volcanisms may have occurred and lasted longer than the mare volcanism.

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The origin of young mare basalts inferred from lunar meteorites Northwest Africa 4734, 032, and LaPaz Icefield 02205

Cited by 64 publications

References 108 publications

Origin of the lunar highlands Mg-suite: An integrated petrology, geochemistry, chronology, and remote sensing perspective

Origin of the lunar highlands Mg-suite: An integrated petrology, geochemistry, chronology, and remote sensing perspective

Magmatic volatiles (H, C, N, F, S, Cl) in the lunar mantle, crust, and regolith: Abundances, distributions, processes, and reservoirs

New Insights Into Lithology Distribution Across the Moon

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