Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

Day, James M.D.; Moynier, Frédéric

doi:10.1098/rsta.2013.0259

Cited by 109 publications

(91 citation statements)

References 99 publications

(341 reference statements)

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“…For example, the degree of depletion of moderately volatile elements in the Moon is similar to that observed for other differentiated and volatile‐depleted planetesimals in the solar system, such as the angrite parent body or Vesta, parent body of eucrites, howardites, and diogenites (e.g., Albarède ; Albarede et al. ; Day and Moynier ). Whether this is related to collisional events or some postaccretion scenarios needs to be more accurately constrained.…”

Section: Introductionsupporting

confidence: 66%

“…For example, the depletion of alkali elements in the Earth relative to chondrites (Palme and O'Neill 2014) as well as that of volatile elements in all planetary materials (Humayun and Clayton 1995) have long been recognized. For example, the degree of depletion of moderately volatile elements in the Moon is similar to that observed for other differentiated and volatile-depleted planetesimals in the solar system, such as the angrite parent body or Vesta, parent body of eucrites, howardites, and diogenites (e.g., Albar ede 2004; Albarede et al 2013;Day and Moynier 2014). Whether this is related to collisional events or some postaccretion scenarios needs to be more accurately constrained.…”

Section: Introductionmentioning

confidence: 71%

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The fate of moderately volatile elements in impact events—Lithium connection between the Ries sediments and central European tektites

Rodovská

Magna

Žák

et al. 2016

Meteorit & Planetary Scien

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Lithium abundances and isotope compositions are presented for a suite of sediments from the surroundings of the Ries Impact structure, paralleled by new Li data for central European tektites (moldavites) from several substrewn fields (South Bohemia, Moravia, Cheb Basin, Lusatia), including a specimen from the newly discovered substrewn field in Poland. The data set was supplemented by three clay fractions isolated from sedimentary samples. Moldavites measured in this study show a very narrow range in δ7Li values (−0.6 to 0.3‰ relative to L‐SVEC) and Li contents (23.9–48.1 ppm). This contrasts with sediments from the Ries area which show remarkable range in Li isotope compositions (from −6.9 to 13.4‰) and Li contents (0.6–256 ppm). The OSM sediments which, based on chemical similarity, formed the major part of moldavites, show a range in δ7Li values from −2.0 to 7.9‰ and Li contents from 5.8 to 78.9 ppm. Therefore, the formation of moldavites was apparently accompanied by large‐scale mixing, paralleled by chemical and isotope homogenization of their parent matter. The proposed Li mixing model indicates that sands, clayey sediments, and low volumes of carbonates are the major components for tektite formation whereas residual paleokarst sediments could have been a minor but important component for a subset of moldavites. Striking homogenization of Li in tektites, combined with limited Li loss during impacts, may suggest that moderately volatile elements are not scavenged and isotopically fractionated during large‐scale collisions, which is consistent with recent models. In general, whether homogenization of bodies with distinct Li isotope systematics takes place, or collision of bodies with similar Li systematics operates cannot be resolved at present stage but Li isotope homogeneity of solar system planets and asteroidal bodies tentatively implies the latter.

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Section: Introductionsupporting

confidence: 66%

Section: Introductionmentioning

confidence: 71%

The fate of moderately volatile elements in impact events—Lithium connection between the Ries sediments and central European tektites

Rodovská

Magna

Žák

et al. 2016

Meteorit & Planetary Scien

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“…This small residual atmosphere may condense or be lost from the Moon. Therefore, in our model, the observed isotopic variability of some volatile elements (e.g., Zn, Cl) in lunar samples (Day & Moynier, ; Paniello et al, ; Sharp et al, ) is unlikely to reflect bulk isotopic fractionation due to atmospheric loss (Day & Moynier, ; Paniello et al, ) and must arise from later, potentially localized, processes.…”

Section: Discussionmentioning

confidence: 88%

The Origin of the Moon Within a Terrestrial Synestia

et al. 2018

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The giant impact hypothesis remains the leading theory for lunar origin. However, current models struggle to explain the Moon's composition and isotopic similarity with Earth. Here we present a new lunar origin model. High‐energy, high‐angular‐momentum giant impacts can create a post‐impact structure that exceeds the corotation limit, which defines the hottest thermal state and angular momentum possible for a corotating body. In a typical super‐corotation‐limit body, traditional definitions of mantle, atmosphere, and disk are not appropriate, and the body forms a new type of planetary structure, named a synestia. Using simulations of cooling synestias combined with dynamic, thermodynamic, and geochemical calculations, we show that satellite formation from a synestia can produce the main features of our Moon. We find that cooling drives mixing of the structure, and condensation generates moonlets that orbit within the synestia, surrounded by tens of bars of bulk silicate Earth vapor. The moonlets and growing moon are heated by the vapor until the first major element (Si) begins to vaporize and buffer the temperature. Moonlets equilibrate with bulk silicate Earth vapor at the temperature of silicate vaporization and the pressure of the structure, establishing the lunar isotopic composition and pattern of moderately volatile elements. Eventually, the cooling synestia recedes within the lunar orbit, terminating the main stage of lunar accretion. Our model shifts the paradigm for lunar origin from specifying a certain impact scenario to achieving a Moon‐forming synestia. Giant impacts that produce potential Moon‐forming synestias were common at the end of terrestrial planet formation.

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“…Of these planetary bodies, the Moon is the most depleted in volatile elements (Day and Moynier 2014;Humayun and Clayton 1995;Paniello et al 2012;Taylor 2001;Taylor et al 2006b), and it is the primary subject of this work.…”

Section: Introductionmentioning

confidence: 99%

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

183

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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Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

Cited by 109 publications

References 99 publications

The fate of moderately volatile elements in impact events—Lithium connection between the Ries sediments and central European tektites

The fate of moderately volatile elements in impact events—Lithium connection between the Ries sediments and central European tektites

The Origin of the Moon Within a Terrestrial Synestia

Magmatic volatiles (H, C, N, F, S, Cl) in the lunar mantle, crust, and regolith: Abundances, distributions, processes, and reservoirs

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