Petrogenesis of picritic mare magmas: Constraints on the extent of early lunar differentiation

Longhi, J.

doi:10.1016/j.gca.2006.09.023

Cited by 125 publications

(103 citation statements)

References 34 publications

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“…Thus the final 'layers' to crystallize from the residual liquid were KREEP-rich (termed urKREEP; [112,113]) and Fe-Ti-rich. It is worth noting that the depth of the LMO is debated to be between 200 and 1000 km [71,114,115] or even whole Moon melting [116][117][118]. The dominant mode of LMO crystallization also remains contentious as to whether it was fractional, equilibrium or a mixture of both [70,119,120].…”

Section: Water In the Lunar Magma Ocean And Mare Basalt Source Regionsmentioning

confidence: 99%

Understanding the origin and evolution of water in the Moon through lunar sample studies

Anand

Tartèse

Barnes

2014

Phil. Trans. R. Soc. A.

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A paradigm shift has recently occurred in our knowledge and understanding of water in the lunar interior. This has transpired principally through continued analysis of returned lunar samples using modern analytical instrumentation. While these recent studies have undoubtedly measured indigenous water in lunar samples they have also highlighted our current limitations and some future challenges that need to be overcome in order to fully understand the origin, distribution and evolution of water in the lunar interior. Another exciting recent development in the field of lunar science has been the unambiguous detection of water or water ice on the surface of the Moon through instruments flown on a number of orbiting spacecraft missions. Considered together, sample-based studies and those from orbit strongly suggest that the Moon is not an anhydrous planetary body, as previously believed. New observations and measurements support the possibility of a wet lunar interior and the presence of distinct reservoirs of water on the lunar surface. Furthermore, an approach combining measurements of water abundance in lunar samples and its hydrogen isotopic composition has proved to be of vital importance to fingerprint and elucidate processes and source(s) involved in giving rise to the lunar water inventory. A number of sources are likely to have contributed to the water inventory of the Moon ranging from primordial water to meteorite-derived water ice through to the water formed during the reaction of solar wind hydrogen with the lunar soil. Perhaps two of the most striking findings from these recent studies are the revelation that at least some portions of the lunar interior are as water-rich as some Mid-Ocean Ridge Basalt source regions on Earth and that the water in the Earth and the Moon probably share a common origin.

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Section: Water In the Lunar Magma Ocean And Mare Basalt Source Regionsmentioning

confidence: 99%

Understanding the origin and evolution of water in the Moon through lunar sample studies

Anand

Tartèse

Barnes

2014

Phil. Trans. R. Soc. A.

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“…Chabot and Agee, 2003), or that current estimates of bulk lunar Cr are too high (e.g. Longhi, 2003Longhi, , 2006Taylor et al, 2006). However, if the symplectites in 76535 formed through an olivine-plagioclase reaction, where diffusion of Cr out of the olivine provided the Cr in the spinel, as has been suggested, the apparent Cr depletion in the olivine is not a primary feature.…”

Section: Introductionmentioning

confidence: 98%

“…The early LMO cumulate component of the Mg-suite source material likely represents dunitic cumulates from the lower cumulate pile that have an Mg * [(molar Mg/[Mg + Fe]) Ã 100] greater than the bulk Moon (bulk Moon Mg * is likely 84-90; i.e. Warren, 2005;Longhi, 2006;Taylor et al, 2006), whereas the late-stage components represent crustal anorthosite and KREEP assimilation (Warren and Wasson, 1979;Warren, 1986Warren, , 1988Papike et al, 1994;Shervais and McGee, 1998;Shearer and Papike, 2005;Elardo et al, 2011). The relationship among Mg-suite samples can be reconstructed through the fractional crystallization sequence dunite !…”

Section: Introductionmentioning

confidence: 99%

Chromite symplectites in Mg-suite troctolite 76535 as evidence for infiltration metasomatism of a lunar layered intrusion

Elardo

McCubbin

Shearer

2012

Geochimica et Cosmochimica Acta

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“…Petrological and geochemical studies of Apollo mare basalts and picritic volcanic glasses have shaped our understanding of the composition and evolution of the lunar mantle (e.g., Taylor, 1975Taylor, , 1982Delano, 1986;Longhi, 1992Longhi, , 2006Taylor et al, 2006). These studies have demonstrated that basaltic magmatism on the Moon is ancient ($4.0 to 2.8 Ga; e.g., Snyder et al, 2000) and compositionally different from that of Earth (Taylor, 1982).…”

Section: Introductionmentioning

confidence: 99%

A laser-ablation ICP-MS study of Apollo 15 low-titanium olivine-normative and quartz-normative mare basalts

Schnare

Day

Norman

et al. 2008

Geochimica et Cosmochimica Acta

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Petrogenesis of picritic mare magmas: Constraints on the extent of early lunar differentiation

Cited by 125 publications

References 34 publications

Understanding the origin and evolution of water in the Moon through lunar sample studies

Understanding the origin and evolution of water in the Moon through lunar sample studies

Chromite symplectites in Mg-suite troctolite 76535 as evidence for infiltration metasomatism of a lunar layered intrusion

A laser-ablation ICP-MS study of Apollo 15 low-titanium olivine-normative and quartz-normative mare basalts

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