A chemical model for generating the sources of mare basalts: Combined equilibrium and fractional crystallization of the lunar magmasphere

Snyder, G. A.; Taylor, L. A.; Neal, C. R.

doi:10.1016/0016-7037(92)90172-f

Cited by 465 publications

(544 citation statements)

References 26 publications

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“…Calculations of µ values of shergottite and Nakhla sources are described in the text and use data from Chen and Wasserburg (1986a;1986b;1993), Misawa et al (1997), Borg et al (2005) 1986;McKenzie and O'Nions, 1991;Beattie, 1993;Ewart and Griffin, 1994;Hauri et al, 1994). Partition coefficients for U are: 0.0001 for olivine, 0.001 for orthopyroxene, 0.02 for clinopyroxene, 0.0001 for garnet, 0.00001 for ilmenite and 0.00001 for sulfide (from: Snyder et al, 1992;Borg and Draper, 2003 Plag = plagioclase, MgPx = Mg-rich pyroxene, FePx = Fe-rich pyroxene, Ox = oxide, Phos = phosphate, Wr = whole rock, (L) = HCl leachate, (R) = residue of HCl leachate, rej = portion of magnetically-separated mineral fraction rejected after hand-picking. a.…”

Section: Discussionmentioning

confidence: 99%

“…4) Borg et al (2003) inferred that the depleted and enriched martian basalt source end-members are analogous to the compositional end-members in the lunar mantle. The lunar mantle end-members are inferred to have formed from crystallization of the lunar magma ocean (e.g., Snyder et al, 1992), and thus Borg et al (2003) proposed that the martian source end-members also formed through crystallization of a magma ocean. In models of the lunar magma ocean, mafic cumulates form a depleted mantle end-member, and late-stage trapped liquid components form an enriched mantle end-member (Snyder et al, 1992).…”

Section: Formation Of the End-member Sources Of Martian Basaltsmentioning

confidence: 99%

“…The lunar mantle end-members are inferred to have formed from crystallization of the lunar magma ocean (e.g., Snyder et al, 1992), and thus Borg et al (2003) proposed that the martian source end-members also formed through crystallization of a magma ocean. In models of the lunar magma ocean, mafic cumulates form a depleted mantle end-member, and late-stage trapped liquid components form an enriched mantle end-member (Snyder et al, 1992). Subsequently, Borg and Draper (2003) presented a petrologic and geochemical model for the formation of these two end- (Borg and Draper, 2003).…”

Section: Formation Of the End-member Sources Of Martian Basaltsmentioning

confidence: 99%

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Uranium–lead isotope systematics of Mars inferred from the basaltic shergottite QUE 94201

Gaffney

Borg

Connelly

2007

Geochimica et Cosmochimica Acta

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Section: Discussionmentioning

confidence: 99%

Section: Formation Of the End-member Sources Of Martian Basaltsmentioning

confidence: 99%

Section: Formation Of the End-member Sources Of Martian Basaltsmentioning

confidence: 99%

See 1 more Smart Citation

Uranium–lead isotope systematics of Mars inferred from the basaltic shergottite QUE 94201

Gaffney

Borg

Connelly

2007

Geochimica et Cosmochimica Acta

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“…[7] Crystallization of an early magma ocean is believed to have resulted in an ultramafic mantle overlaid by an anorthositic crust [e.g., Wood et al, 1970, Snyder et al, 1992Hess and Parmentier, 1995;Elkins-Tanton et al, 2011]. On average, the crust is~40 km thick, as shown by recent models incorporating Gravity Recovery and Interior Laboratory (GRAIL) gravity and Lunar Orbiter Laser Altimeter (LOLA) topography data [Wieczorek et al, 2013].…”

Section: The Evolution and Stratigraphy Of The Lunar Crust And Mantlementioning

confidence: 99%

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

2013

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[1] Using high-spectral and -spatial resolution Moon Mineralogy Mapper data, we investigate compositional variations across the central peak structures of four impact craters within the South Pole-Aitken Basin (SPA). Two distinct causes of spectral diversity are observed. Spectral variations across the central peaks of Bhabha, Finsen, and Lyman are dominated by soil development, including the effects of space weathering and mixing with local materials. For these craters, the central peak structure is homogeneous in composition, although small compositional differences between the craters are observed. This group of craters is located within the estimated transient cavity of SPA, and their central uplifts exhibit similar mafic abundances. Therefore, it is plausible that they have all uplifted material associated with melts of the lower crust or upper mantle produced during the SPA impact. Compositional differences observed between the peaks of these craters reflect heterogeneities in the SPA subsurface, although the origin of this heterogeneity is uncertain. In contrast to these craters, Leeuwenhoek exhibits compositional heterogeneity across its central peak structure. The peak is areally dominated by feldspathic materials, interspersed with several smaller exposures exhibiting a mafic spectral signature. Leeuwenhoek is the largest crater included in the study and is located in a region of complex stratigraphy involving both crustal (feldspathic) and SPA (mafic melt and ejecta) materials. The compositional diversity observed in Leeuwenhoek's central peak indicates that kilometer-scale heterogeneities persist to depths of more than 10 km in this region.

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“…3, 8, 15, and 16). Following the initial stages of lunar accretion, the lunar-wide magma ocean began to cool and crystallize, marking the start of lunar magmatism and differentiation (21)(22)(23)(24)(25). During lunar magma ocean crystallization, it is believed that early-forming ferromagnesian minerals (olivine and pyroxene) sank to the magma ocean floor, resulting in a lunar mantle composed of stratified cumulate mineral layers (21 -25).…”

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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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A chemical model for generating the sources of mare basalts: Combined equilibrium and fractional crystallization of the lunar magmasphere

Cited by 465 publications

References 26 publications

Uranium–lead isotope systematics of Mars inferred from the basaltic shergottite QUE 94201

Uranium–lead isotope systematics of Mars inferred from the basaltic shergottite QUE 94201

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

Nominally hydrous magmatism on the Moon

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