Early crustal building processes on the moon: Models for the petrogenesis of the magnesian suite

Shearer, C. K.; Papike, J. J.

doi:10.1016/j.gca.2005.02.025

Cited by 112 publications

(134 citation statements)

References 50 publications

(114 reference statements)

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“…S1, adapted from ref. 45). In addition to the two pyroxenes and the plagioclase, abundant K-rich feldspar and minor silica, fluorapatite, merrillite, Cr-rich spinel, and Fe-Ti oxides are also present in the clast.…”

Section: Resultsmentioning

confidence: 99%

Nominally hydrous magmatism on the Moon

McCubbin

Steele

Hauri

et al. 2010

Proc. Natl. Acad. Sci. U.S.A.

275

185

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For the past 40 years, the Moon has been described as nearly devoid of indigenous water; however, evidence for water both on the lunar surface and within the lunar interior have recently emerged, calling into question this long-standing lunar dogma. In the present study, hydroxyl (as well as fluoride and chloride) was analyzed by secondary ion mass spectrometry in apatite [Ca 5 ðPO 4 Þ 3 ðF,Cl,OHÞ] from three different lunar samples in order to obtain quantitative constraints on the abundance of water in the lunar interior. This work confirms that hundreds to thousands of ppm water (of the structural form hydroxyl) is present in apatite from the Moon. Moreover, two of the studied samples likely had water preserved from magmatic processes, which would qualify the water as being indigenous to the Moon. The presence of hydroxyl in apatite from a number of different types of lunar rocks indicates that water may be ubiquitous within the lunar interior, potentially as early as the time of lunar formation. The water contents analyzed for the lunar apatite indicate minimum water contents of their lunar source region to range from 64 ppb to 5 ppm H 2 O. This lower limit range of water contents is at least two orders of magnitude greater than the previously reported value for the bulk Moon, and the actual source region water contents could be significantly higher. O ne of the scientific discoveries resulting from the Apollo missions was the pervasive waterless nature of the Moon and its rocks. The initial studies of the returned samples were pristine and showed no evidence of aqueous alteration, and water analyses were below detection limits. Moreover, hydrous phases were absent from the lunar rocks aside from a few unconfirmed reports of possible amphibole grains (1), which are now considered by many to represent either misidentifications or terrestrial contamination (as summarized by ref. 2). The subsequent forty years of lunar sample analysis have only supported and strengthened the idea that indigenous water was nearly absent from the Moon's interior. In fact, this conclusion has been incorporated into many petrologic and geophysical models constructed to aid in our understanding of lunar formation and lunar geology (3-11). The bulk water content of the Moon was recently estimated to be less than 1 ppb (11), which would make the Moon at least six orders of magnitude drier than the interiors of Earth (12, 13) and Mars (14). This extremely low water content is in keeping with the pervasive volatile-element depletion signature recorded in all lunar materials, because hydrogen is the most volatile of the elements. The exact cause for this volatile-element depletion is still under question; however, many have argued that it stems from the high temperatures associated with the Moon-forming giant-impact event at ∼4.5 Ga (i.e., refs. 3,8,15,and 16).Facilitated by advancements in analytical detection sensitivities for water, several recent discoveries have indicated that the story of water on the Moon is far from complete. Evi...

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Section: Resultsmentioning

confidence: 99%

Nominally hydrous magmatism on the Moon

McCubbin

Steele

Hauri

et al. 2010

Proc. Natl. Acad. Sci. U.S.A.

275

185

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“…In a nutshell, the dense, KREEP-rich, Fe-Ti-rich material sank through the LMO cumulate pile and probably triggered the onset of Mgrich basaltic magmatism (i.e. onset of Mg-suite and alkali-suite magmatism [123,124]). However, it is not known as to how much mixing of interior material was achieved by the overturn event.…”

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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“…This group of highlands rocks is known as the Mg-suite [7]. The parental magmas to the Mg-suite cumulate rocks usually are assumed to be partial melts of cumulates in the lunar interior [8], although an alternative is that the parental magmas originate from large impacts [9].…”

Section: Introductionmentioning

confidence: 99%

“…Finally, exposure of the lunar surface to cosmic ray irradiation produces secondary neutrons that can substantially influence the isotopic composition of samples that have long exposure histories, with important consequences for 146 Sm- 142 Nd and Lu-Hf results [31][32][33][34][35]. (8) 67075 (7) 60025 (6) 67215 (4) Y86032 (5) 60025 (3) 62236 (1) 60016, 3A (2) (a) (9) 73255 (10) 15445,247 (11) 76535 (12) 76355 (13) 76535 (14) 77215 (15) 77215 (16) 78238 (17) 78236 (10) 78236 (18) 15445, 17 (11) FAN range [12]; 2-Marks et al [13]; 3-Borg et al [14]; 4-Norman et al [15]; 5-Nyquist et al [16]; 6-Carlson & Lugmair [17]; 7-Nyquist et al [18]; 8-Alibert et al [19]; 9-Carlson & Lugmair [20]; 10-Carlson & Lugmair [21]; 11-Shih et al [22]; 12-Lugmair et al [23]; 13-Edmunson et al [24]; 14-Borg et al [25]; 15-this study; 16-Nakamura et al [26]; 17-Edmunson et al [27] and 18-Nyquist et al [28]. of lunar highlands rocks.…”

Section: Introductionmentioning

confidence: 99%

Rb-Sr, Sm-Nd and Lu-Hf isotope systematics of the lunar Mg-suite: the age of the lunar crust and its relation to the time of Moon formation

Carlson

Borg

Gaffney

et al. 2014

Phil. Trans. R. Soc. A.

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New Rb-Sr, 146,147 143 Nd and Lu-Hf isotopic analyses of Mg-suite lunar crustal rocks 67667, 76335, 77215 and 78238, including an internal isochron for norite 77215, were undertaken to better define the time and duration of lunar crust formation and the history of the source materials of the Mg-suite. Isochron ages determined in this study for 77215 are: Rb-Sr = 4450 ± 270 Ma, 147 Sm-143 Nd = 4283 ± 23 Ma and Lu-Hf = 4421 ± 68 Ma. The data define an initial 146 Sm/ 144 Sm ratio of 0.00193 ± 0.00092 corresponding to ages between 4348 and 4413 Ma depending on the halflife and initial abundance used for 146 Sm. The initial Nd and Hf isotopic compositions of all samples indicate a source region with slight enrichment in the incompatible elements in accord with previous suggestions that the Mg-suite crustal rocks contain a component of KREEP. The Sm/Nd-142

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Early crustal building processes on the moon: Models for the petrogenesis of the magnesian suite

Cited by 112 publications

References 50 publications

Nominally hydrous magmatism on the Moon

Nominally hydrous magmatism on the Moon

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

Rb-Sr, Sm-Nd and Lu-Hf isotope systematics of the lunar Mg-suite: the age of the lunar crust and its relation to the time of Moon formation

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