The hydrogen isotopic composition of lunar melt inclusions: An interplay of complex magmatic and secondary processes

Stephant, A.; Anand, M.; Tartèse, Romain; Zhao, X.; Degli-Alessandrini, G.; Franchi, I. A.

doi:10.1016/j.gca.2020.06.017

Cited by 22 publications

(31 citation statements)

References 121 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These observations provide convincing evidence that ilmenite-hosted melt inclusions recorded the progressive evolution of melts undergoing degassing of H 2 , resulting in considerable D-enrichment during crystallisation of the CE5 basalts 15,39 . Diffusion out of the melt inclusions is another process by D/H ratios can be fractionated as reported for melt inclusions enclosed in olivine and pyroxene from Apollo basalts 11 . At present there is no constraints on diffusion rate of water in ilmenite-hosted melt inclusions.…”

mentioning

confidence: 96%

mentioning

confidence: 99%

See 1 more Smart Citation

A dry lunar mantle reservoir for young mare basalts of Chang’e-5

et al. 2021

Nature

Self Cite

140

View full text Add to dashboard Cite

The distribution of water in the Moon's interior carries key implications for the origin of the Moon 1 , the crystallisation of the lunar magma ocean 2 , and the duration of lunar volcanism 2 . The Chang'E-5 (CE5) mission returned the youngest mare basalt samples, dated at ca. 2.0 billion years ago 3 , from the northwestern Procellarum KREEP Terrane (PKT), providing a probe into the spatio-temporal evolution of lunar water. Here we report the water abundance and hydrogen isotope composition of apatite and ilmenite-hosted melt inclusions from CE5 basalts, from which we derived a maximum water abundance of 370 ± 30 g.g -1 and a δD value (-330 ± 160‰) for their parent magma. During eruption, hydrogen degassing led to an increase in the D/H ratio of the residual melts up to δD values of 300-900‰. Accounting for low degrees of mantle partial melting followed by extensive magma fractional crystallisation 4 , we estimate a maximum mantle water abundance of 2-6 g.g -1 , which are too low for water contents alone to account for generating the Moon's youngest basalts. Such modest water abundances for the lunar mantle are at the lower end of those estimated from mare basalts that erupted from ca. 4.0-2.8 Ga 5, 6 , suggesting the mantle source of CE5 basalts dried up by ca. 2.0 Ga through previous melt extraction from the PKT mantle during prolonged volcanic activity.Water abundance in the lunar mantle places strict constraints on high-temperature processes, including the Moon-forming giant impact 1 , the ensuing crystallisation of the lunar magma ocean 7 , and the longevity of volcanism on the Moon 2 . Based upon the analyses carried out since the Apollo era, the Moon was long thought to be an anhydrous body. Advances in in situ analytical techniques over the past decade have allowed analysis of water abundances at micro-scale in various lunar samples, including in olivine-and pyroxene-hosted melt inclusions in mare basalts [8][9][10][11][12] , apatite in mare basalts and highlands samples [13][14][15][16][17][18][19][20] , pyroclastic glass beads 21, 22 , and

show abstract

mentioning

confidence: 96%

mentioning

confidence: 99%

A dry lunar mantle reservoir for young mare basalts of Chang’e-5

et al. 2021

Nature

Self Cite

140

View full text Add to dashboard Cite

show abstract

“…Here, we define volatile elements as those with 50% condensation temperatures below these of the major rock-forming elements Fe, Mg, and Si (6). This paradigm shift was accompanied by new measurements of volatile stable isotope compositions (e.g., H, C, N, Cl, K, Cr, Cu, Zn, Ga, Rb, and Sn) in a wealth of bulk lunar samples (7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18) and in the mineral phases and melt inclusions they host (19)(20)(21)(22)(23)(24)(25)(26)(27)(28). These studies have shown that the stable isotope compositions of most MVEs (e.g., K, Zn, Ga, and Rb) are enriched in their heavier isotopes with respect to the bulk silicate Earth (BSE) (9,11,(13)(14)(15)17).…”

mentioning

confidence: 99%

Conditions and extent of volatile loss from the Moon during formation of the Procellarum basin

Tartèse

Sossi

Moynier

2021

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

Self Cite

View full text Add to dashboard Cite

Rocks from the lunar interior are depleted in moderately volatile elements (MVEs) compared to terrestrial rocks. Most MVEs are also enriched in their heavier isotopes compared to those in terrestrial rocks. Such elemental depletion and heavy isotope enrichments have been attributed to liquid–vapor exchange and vapor loss from the protolunar disk, incomplete accretion of MVEs during condensation of the Moon, and degassing of MVEs during lunar magma ocean crystallization. New Monte Carlo simulation results suggest that the lunar MVE depletion is consistent with evaporative loss at 1,670 ± 129 K and an oxygen fugacity +2.3 ± 2.1 log units above the fayalite-magnetite-quartz buffer. Here, we propose that these chemical and isotopic features could have resulted from the formation of the putative Procellarum basin early in the Moon’s history, during which nearside magma ocean melts would have been exposed at the surface, allowing equilibration with any primitive atmosphere together with MVE loss and isotopic fractionation.

show abstract

“…Based upon the analyses carried out since the Apollo era, the Moon was long thought to be an anhydrous body. Advances in in situ analytical techniques over the past decade have allowed analysis of water abundances at micro-scale in various lunar samples, including in olivine-and pyroxene-hosted melt inclusions in mare basalts [8][9][10][11][12] , apatite in mare basalts and highlands samples [13][14][15][16][17][18][19][20] , pyroclastic glass beads 21,22 , and anorthosites 23, . The estimates of water abundances for their mantle source regions span a wide range from ~0.3 to 200 g.g -1 25 , suggesting that the Moon's interior is not as anhydrous as previously thought.…”

mentioning

confidence: 99%

“…This large range of estimates could also be affected by the mixing of endogenous water with various exogenic water sources, i.e. asteroids, comets, and solar wind 19,26,27 , and/or by interplay between many processes, such as volatile degassing, partial melting, fractional crystallisation, impacting, mixing with potassium (K), rare earth elements (REE) and phosphorus (P) (KREEP)-rich components, and spallation 11,15,25,[27][28][29] . It is thus crucial to combine in situ analysis of water abundances and hydrogen isotope composition with detailed contextual petrographic information.The Chang'E-5 (CE5) mission successfully returned 1.731 kg of lunar soil samples from young mare basalt units dated at ca.…”

mentioning

confidence: 99%

A dry lunar mantle reservoir for young mare basalts of Chang’E-5

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

The distribution of water in the Moon’s interior carries key implications for the origin of the Moon1, the crystallisation of the lunar magma ocean2, and the duration of lunar volcanism2. The Chang’E-5 (CE5) mission returned the youngest mare basalt samples, dated at ca. 2.0 billion years ago3, from the northwestern Procellarum KREEP Terrane (PKT), providing a probe into the spatio-temporal evolution of lunar water. Here we report the water abundance and hydrogen isotope composition of apatite and ilmenite-hosted melt inclusions from CE5 basalts, from which we derived a maximum water abundance of 370 ± 30 μg.g-1 and a δD value (-330 ± 160‰) for their parent magma. During eruption, hydrogen degassing led to an increase in the D/H ratio of the residual melts up to δD values of 300-900‰. Accounting for low degrees of mantle partial melting followed by extensive magma fractional crystallisation4, we estimate a maximum mantle water abundance of 2-6 μg.g-1, which are too low for water contents alone to account for generating the Moon’s youngest basalts. Such modest water abundances for the lunar mantle are at the lower end of those estimated from mare basalts that erupted from ca. 4.0-2.8 Ga5, 6, suggesting the mantle source of CE5 basalts dried up by ca. 2.0 Ga through previous melt extraction from the PKT mantle during prolonged volcanic activity.

show abstract

The hydrogen isotopic composition of lunar melt inclusions: An interplay of complex magmatic and secondary processes

Cited by 22 publications

References 121 publications

A dry lunar mantle reservoir for young mare basalts of Chang’e-5

A dry lunar mantle reservoir for young mare basalts of Chang’e-5

Conditions and extent of volatile loss from the Moon during formation of the Procellarum basin

A dry lunar mantle reservoir for young mare basalts of Chang’E-5

Contact Info

Product

Resources

About