Formation of Apollo 16 impactites and the composition of late accreted material: Constraints from Os isotopes, highly siderophile elements and sulfur abundances

Gleißner, Philipp; Becker, Harry

doi:10.1016/j.gca.2016.12.017

Cited by 20 publications

(37 citation statements)

References 61 publications

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“…; Day et al. ; Gleißner and Becker ). A persistent concern is potential metal contamination during curation and curatorial sample processing due to the significant leverage of high HSE abundances (10s–100s ng g −1 ) in the stainless steel tools compared with pristine crustal rocks or mare basalts (0.001–0.1s ng g −1 ), or impact melt rocks (1–10s ng g −1 ).…”

Section: Discussionmentioning

confidence: 99%

The potential for metal contamination during Apollo lunar sample curation

Day

Maria-Benavides

McCubbin

et al. 2018

Meteorit & Planetary Scien

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Curation and preparation of samples for chemical analysis can occasionally lead to significant contamination. This issue is of concern in the study of lunar samples, especially those from the Apollo sample collection, where available masses are finite. Here we present compositional data for stainless steels that have commonly been used in the processing of Apollo lunar samples at NASA Johnson Space Center, including a chisel and a vessel typically used to transfer Apollo samples to principal investigators. The Type 304 stainless steels are Cr‐rich, with high concentrations of Mn (4000–18,000 μg g−1), Cu (1000–22,900 μg g−1), Mo (1030–1120 μg g−1), and W (72–193 μg g−1). They have elevated highly siderophile element (HSE) concentrations (up to 92 ng g−1 Os), 187Os/188Os ranging from 0.1310 to 0.1336, and negligible lithophile element abundances. We find that, while metal contamination is possible, significant (≫0.01% by mass) addition of stainless steel is required to strongly affect the composition of the HSE, W, Mo, Cr, or Cu for most Apollo lunar samples. Nonetheless, careful appraisal on a case‐by‐case basis should take place to ensure contamination introduced through sample processing during curation is at acceptably low levels. A survey of lunar mare basalts and crustal rocks indicates that metal contamination plays a negligible role in the compositional variability of the HSE and W compositions preserved in these samples. Further work to constrain contamination for other properties of Apollo samples is required (e.g., organics, microbes, water, noble gases, and magnetics), but the effect of metal contamination can be well‐constrained for the Apollo lunar collection.

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Section: Discussionmentioning

confidence: 99%

The potential for metal contamination during Apollo lunar sample curation

Day

Maria-Benavides

McCubbin

et al. 2018

Meteorit & Planetary Scien

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“…Volatile elements (H, C, N, S) and HSE abundances and isotopic compositions of lunar regolith and impact-melt samples provide indirect evidence for the types of impactors involved. Analysis of Apollo 14, 15, 16 and 17 samples show a broadly linear correlation between HSE/Ir and 187 Os/ 188 Os signatures (Puchtel et al 2008;Fischer-Gödde and Becker 2012;Sharp et al 2014;Gleißner and Becker 2017), reflecting the addition of chondritic and non-chondritic components to the lunar crust, the non-chondritic component HSE composition resembling that of iron meteorites, and contributing up to ∼30 wt.% HSE in the most fractionated Apollo 16 impact-melt samples (e.g., Gleißner and Becker 2017). Siderophile element abundances in mature regolith samples that have been exposed at the lunar surface for hundreds of millions of years suggest the addition of ca.…”

Section: Sources Of Impactorsmentioning

confidence: 92%

Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples

et al. 2019

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The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scientific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to containing a treasure trove of the Moon's history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently available samples, such as those related to the age of the Moon, duration of lunar volcanism, the

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“…Being a dominant phosphide phase in the metal-rich part of the Fe-Ni-P(S) system, schreibersite is a regular subject of studies devoted to evolution of planetary interiors (e.g., Clarke and Goldstein 1978;Scott et al 2007;Goldstein et al 2009;Gu et al 2014Gu et al , 2016He et al 2019; Khisina et al 2019;Chabot et al 2020;Chornkrathok et al 2020). The mineral is a typical constituent of enstatite chondrites and achondrites (Wasson and Wai 1970); it was encountered in carbonaceous chondrites (Zolensky et al 2002), acapulcoites, lodranites and winonaites (Li et al 2011; Keil and McCoy 2018) and in Lunar rocks (Smith and Steele 1976;Gleißner and Becker 2017). Thermodynamic calculations evidence that schreibersite could be a primary phosphorusbearing phase formed during solar nebula condensation (Pasek 2008).…”

Section: Introductionmentioning

confidence: 99%

Crystal chemistry of schreibersite, (Fe,Ni)3P

Britvin

Krzhizhanovskaya

Zolotarev

et al. 2021

American Mineralogist

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Schreibersite, (Fe,Ni)3P, the most abundant cosmic phosphide, is a principal carrier of phosphorus in the natural Fe-Ni-P system and a likely precursor for prebiotic organophosphorus compounds at the early stages of Earth’s evolution. The crystal structure of the mineral contains three metal sites allowing for unrestricted substitution of Fe for Ni. The distribution of these elements across the structure could serve as a tracer of crystallization conditions of schreibersite and its parent celestial bodies. However, discrimination between Fe (Z = 26) and Ni (Z = 28) based on the conventional X-ray structural analysis was for a long time hampered due to the proximity of their atomic scattering factors. We herein show that this problem has been overcome with the implementation of area detectors in the practice of X-ray diffraction. We report on previously unknown site-specific substitution trends in schreibersite structure. The composition of the studied mineral encompasses a Ni content ranging between 0.03 and 1.54 Ni atoms per formula unit (apfu): the entire Fe-dominant side of the join Fe3P-Ni3P. Of 23 schreibersite crystals studied, 22 comprise magmatic and non-magmatic iron meteorites and main group pallasites. The near end-member mineral (0.03 Ni apfu) comes from the pyrometamorphic rocks of the Hatrurim Basin, Negev desert, Israel. It was found that Fe/Ni substitution in schreibersite follows the same trends in all studied meteorites. The dependencies are nonlinear and can be described by second-order polynomials. However, the substitution over the M2 and M3 sites within the most common range of compositions (0.6 < Ni <1.5 apfu) is well approximated by a linear regression: Ni(M2) = 0.84 × Ni(M3) – 0.30 apfu (standard error 0.04 Ni apfu). The analysis of the obtained results shows a strong divergence between the variation of unit-cell parameters of natural schreibersite and those of synthetic (Fe,Ni)3P. This indicates that Fe/Ni substitution trends in the mineral and its synthetic surrogates are different. A plausible explanation might be related to the differences in the system equilibration time of meteoritic schreibersite (millions of years) and synthetic (Fe,Ni)3P (~100 days). However, regardless of the reason for the observed difference, synthetic (Fe,Ni)3P cannot be considered a structural analog of natural schreibersite, and this has to be taken into account when using synthetic (Fe,Ni)3P as an imitator of schreibersite in reconstructions of natural processes.

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Formation of Apollo 16 impactites and the composition of late accreted material: Constraints from Os isotopes, highly siderophile elements and sulfur abundances

Cited by 20 publications

References 61 publications

The potential for metal contamination during Apollo lunar sample curation

The potential for metal contamination during Apollo lunar sample curation

Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples

Crystal chemistry of schreibersite, (Fe,Ni)3P

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