Solar wind nitrogen and indigenous nitrogen in lunar material

Müller, O.

doi:10.1016/0079-1946(79)90007-7

Cited by 5 publications

(8 citation statements)

References 9 publications

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“…The hydrogen isotope compositions of bulk soil samples are largely consistent with SW origin with highly depleted D/H values (e.g., Epstein and Taylor 1970b, 1974Friedman et al 1970aFriedman et al , 1970bFriedman et al , 1972Merlivat et al 1974;Stievenard et al 1990). However, abundances of D in some samples are higher than expected from spallation D generated from solar-and galacticcosmic ray bombardments (e.g., Taylor 1970b, 1972;Friedman et al 1972;Stephant and Robert 2014;Stievenard et al 1990).…”

Section: Volatiles In the Lunar Megaregolithmentioning

confidence: 86%

“…The carbon contents in lunar soils and regolith breccias can reach up to 280 ppm C, with an average of ~100 to 150 ppm among soils from different missions (summary table A8.6 in Haskin and Warren 1991). The nitrogen contents among lunar soils and regolith breccias range from 4 to 209 ppm, generally higher than in lunar rocks by one to two orders of magnitude (Haskin and Warren 1991;Mathew and Marti 2001;Muller 1974). Early studies of lunar regolith observed coupled increases in carbon and nitrogen abundances, suggesting a common source.…”

Section: Volatiles In the Lunar Megaregolithmentioning

confidence: 96%

“…Magmatic troilite is typically found as discrete grains or in late-stage mesostasis pockets, sometimes intergrown with Fe-metal (e.g., Skinner 1970). Vapor or fluid deposited troilite is often found to fill cracks or as intergrowths (Boyce et al 2010;Butler and Meyer 1976;Duncan et al 1973;Fegley and Swindle 1993;Gibson and Moore 1974;Goldberg et al 1976;Haskin and Warren 1991;Hauri et al 2011;Jovanovic et al 1976;Reed 1973, 1975;Liu et al 2012a;Mathew and Marti 2001;McCubbin et al 2011McCubbin et al , 2010bMortimer et al 2015;Muller 1974;Jovanovic 1973a, 1973b;Reed et al 1977;Saal et al 2008;Tartèse et al , 2014aTaylor et al 2004;Wang et al 2012;Wänke et al 1976). a When only an upper value is given, the lower bound value reported is below analytical detection, otherwise a range is reported.…”

Section: Volatile-bearing Mineralogymentioning

confidence: 97%

“…S abundances of mare basalts range from approximately 300 to 3200 ppm Haskin and Warren 1991; Table 2). Mare basalts typically contain less than 1 ppm of indigenous N (Becker et al 1976;Des Marais 1978Mathew and Marti 2001;Mortimer et al 2015;Muller 1974), which has hampered measurement efforts to date, but N abundances have been measured as high as 20 ppm N (Haskin and Warren 1991). Similar to N and H, there is much debate over the indigenous inventory of C in lunar basalts vs. the fraction that can be attributed to secondary processes.…”

Section: Volatiles Within Volcanic Rocksmentioning

confidence: 98%

“…N in mare basalts and pyroclastic glasses. Lunar rocks contain much less N than soils, typically less than 1 ppm of indigenous N (Becker et al 1976;Des Marais 1978Mathew and Marti 2001;Mortimer et al 2015;Muller 1974), which has hampered measurement efforts to date. At such low abundances, indigenous lunar isotopic signatures are masked by those of cosmogenic components (Mathew and Marti 2001).…”

Section: Isotopic Data For Volatile Elementsmentioning

confidence: 99%

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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

178

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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