Evolution, Lunar: From Magma Ocean to Crust Formation

Gross, J.; Joy, Katherine H.

doi:10.1007/978-3-319-05546-6_39-1

Cited by 21 publications

(20 citation statements)

References 134 publications

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“…) suggesting that the samples investigated in this study were formed of lithologies not associated with the nearside KREEP‐rich Procellarum KREEP Terrane (where regoliths typically have >2 ppm Th; see Fig. of Gross and Joy ). Likewise the samples are not from a region bearing alkali‐suite, KREEP basalts, incompatible trace element‐rich impact melts, or mare basalts as these lithologies are not petrographically or mineralogically observed in the samples.…”

Section: Discussionmentioning

confidence: 88%

Investigating the shock histories of lunar meteorites Miller Range 090034, 090070, and 090075 using petrography, geochemistry, and micro‐FTIR spectroscopy

Martín

Pernet‐Fisher

Joy

et al. 2017

Meteorit & Planetary Scien

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Abstract-Fourier transform infrared (FTIR) spectroscopy and cathodoluminescence (CL) imaging techniques, combined with electron microprobe analyses, have been used to determine the physical state of feldspathic phases that have been subject to varying levels of shock in the grouped lunar meteorites Miller Range 090034, 090070, and 090075. Six feldspathic phases have been identified based on spectral, textural, and chemical properties. A specific infrared wavelength band ratio (1064/932 cm À1 equivalent to 9.40/10.73 lm), chosen because it can distinguish between some of the feldspathic phases, can be used to estimate the pressure regimes experienced by these phases. In addition, FTIR spatial mapping capabilities allow for visual comparison of variably shocked phases within the samples. By comparing spectral and compositional data, the origin and shock history of this lunar meteorite group has been determined, with each of the shocked feldspathic phases being related to events in its geological evolution. As such, we highlight that FTIR spectroscopy can be easily employed to identify shocked feldspathic phases in lunar samples; estimate peak shock pressures; and when compared with chemical data, can be used to investigate their shock histories.

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Section: Discussionmentioning

confidence: 88%

Investigating the shock histories of lunar meteorites Miller Range 090034, 090070, and 090075 using petrography, geochemistry, and micro‐FTIR spectroscopy

Martín

Pernet‐Fisher

Joy

et al. 2017

Meteorit & Planetary Scien

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“…The last phases to solidify in the impact-induced Lunar Magma Ocean (LMO) were K-, REE-, and P-rich residual components (urKREEP) and complementarily an ilmenite-bearing cumulate (IBC;Warren and Wasson, 1979;Snyder et al, 1992). Subsequent magmatic processes concluded with the eruption of lunar mare basalts (e.g., Gross and Joy, 2016). Experimental studies and the Hf and Nd isotope composition of mare basalts suggest that low-Ti mare basalts likely result from partial melting of lunar mafic cumulates, whereas high-Ti mare basalts are thought to reflect IBC involvement (e.g., Longhi, 1992;Sprung et al, 2013).…”

Section: Introductionmentioning

confidence: 99%

Unravelling lunar mantle source processes via the Ti isotope composition of lunar basalts

Horan¹,

Hilton

McCoy-West

et al. 2020

Geochem. Persp. Let.

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Formation and crystallisation of the Lunar Magma Ocean (LMO) was one of the most incisive events during the early evolution of the Moon. Lunar Magma Ocean solidification concluded with the coeval formation of K-, REE-and P-rich components (KREEP) and an ilmenite-bearing cumulate (IBC) layer. Gravitational overturn of the lunar mantle generated eruptions of basaltic rocks with variable Ti contents, of which their δ 49 Ti variations may now reflect variable mixtures of ambient lunar mantle and the IBC. To better understand the processes generating the spectrum of lunar low-Ti and high-Ti basalts and the role of Ti-rich phases such as ilmenite, we determined the mass dependent Ti isotope composition of four KREEP-rich samples, 12 low-Ti, and eight high-Ti mare basalts by using a 47 Ti-49 Ti double spike. Our data reveal significant variations in δ 49 Ti for KREEPrich samples (+0.117 to +0.296 ‰) and intra-group variations in the mare basalts (-0.030 to +0.055 ‰ for low-Ti and +0.009 to +0.115 ‰ for high-Ti basalts). We modelled the δ 49 Ti of KREEP using previously published HFSE data as well as the δ 49 Ti evolution during fractional crystallisation of the LMO. Both approaches yield δ 49 Ti KREEP similar to measured values and are in excellent agreement with previous studies. The involvement of ilmenite in the petrogenesis of the lunar mare basalts is further evaluated by combining our results with element ratios of HFSE, U and Th, revealing that partial melting in an overturned lunar mantle and fractional crystallisation of ilmenite must be the main processes accounting for mass dependent Ti isotope variations in lunar basalts. Based on our results we can also exclude formation of high-Ti basalts by simple assimilation of ilmenite by ascending melts from the depleted lunar mantle. Rather, our data are in accord with melting of these basalts from a hybrid mantle source formed in the aftermath of gravitational lunar mantle overturn, which is in good agreement with previous Fe isotope data.

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“…; Elkins‐Tanton et al. ; Gross and Joy ; Pernet‐Fisher and Joy ) and ancient magmatic intrusions such as the high‐Mg suite (HMS) and the high‐Alkali suite formed ~4500 to 4100 Ma, and 4370–4030 Ma (extending to 3800 Ma), respectively (Carlson and Lugmair ; Meyer et al. , ; Nyquist and Shih ; Nyquist et al.…”

Section: Introductionmentioning

confidence: 99%

“…The age of the oldest known volcanic sample at 4350 Ma (Kalahari 009: Terada et al 2007), implies an overlap between the beginning of lunar basaltic volcanism with ancient feldspathic crustal rocks. For example, the ferroan anorthosites (FAN), formed 4560-4280 Ma (Carlson and Lugmair 1988;Nyquist et al 1995Nyquist et al , 2010Borg et al 1999Borg et al , 2011Nemchin et al 2009a;Elkins-Tanton et al 2011;Gross and Joy 2016;Pernet-Fisher and Joy 2016) and ancient magmatic intrusions such as the high-Mg suite (HMS) and the high-Alkali suite formed~4500 to 4100 Ma, and 4370-4030 Ma (extending to 3800 Ma), respectively (Carlson and Lugmair 1981;Meyer et al 1989Meyer et al , 1996Nyquist and Shih 1992;Nyquist et al 2010;Borg et al 2011;Carlson et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The early geological history of the Moon inferred from ancient lunar meteorite Miller Range 13317

Curran

Joy

Snape

et al. 2019

Meteorit & Planetary Scien

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Miller Range (MIL) 13317 is a heterogeneous basalt‐bearing lunar regolith breccia that provides insights into the early magmatic history of the Moon. MIL 13317 is formed from a mixture of material with clasts having an affinity to Apollo ferroan anorthosites and basaltic volcanic rocks. Noble gas data indicate that MIL 13317 was consolidated into a breccia between 2610 ± 780 Ma and 1570 ± 470 Ma where it experienced a complex near‐surface irradiation history for ~835 ± 84 Myr, at an average depth of ~30 cm. The fusion crust has an intermediate composition (Al2O3 15.9 wt%; FeO 12.3 wt%) with an added incompatible trace element (Th 5.4 ppm) chemical component. Taking the fusion crust to be indicative of the bulk sample composition, this implies that MIL 13317 originated from a regolith that is associated with a mare‐highland boundary that is KREEP‐rich (i.e., K, rare earth elements, and P). A comparison of bulk chemical data from MIL 13317 with remote sensing data from the Lunar Prospector orbiter suggests that MIL 13317 likely originated from the northwest region of Oceanus Procellarum, east of Mare Nubium, or at the eastern edge of Mare Frigoris. All these potential source areas are on the near side of the Moon, indicating a close association with the Procellarum KREEP Terrane. Basalt clasts in MIL 13317 are from a very low‐Ti to low‐Ti (between 0.14 and 0.32 wt%) source region. The similar mineral fractionation trends of the different basalt clasts in the sample suggest they are comagmatic in origin. Zircon‐bearing phases and Ca‐phosphate grains in basalt clasts and matrix grains yield 207Pb/206Pb ages between 4344 ± 4 and 4333 ± 5 Ma. These ancient 207Pb/206Pb ages indicate that the meteorite has sampled a range of Pre‐Nectarian volcanic rocks that are poorly represented in the Apollo, Luna, and lunar meteorite collections. As such, MIL 13317 adds to the growing evidence that basaltic volcanic activity on the Moon started as early as ~4340 Ma, before the main period of lunar mare basalt volcanism at ~3850 Ma.

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Evolution, Lunar: From Magma Ocean to Crust Formation

Cited by 21 publications

References 134 publications

Investigating the shock histories of lunar meteorites Miller Range 090034, 090070, and 090075 using petrography, geochemistry, and micro‐FTIR spectroscopy

Investigating the shock histories of lunar meteorites Miller Range 090034, 090070, and 090075 using petrography, geochemistry, and micro‐FTIR spectroscopy

Unravelling lunar mantle source processes via the Ti isotope composition of lunar basalts

The early geological history of the Moon inferred from ancient lunar meteorite Miller Range 13317

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