¹Qin Zhou et al. (>10)
Geochimica et Cosmochimica Acta (in Press) Open Access Link to Article [https://doi.org/10.1016/j.gca.2023.08.017]
¹Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
Copyright Elsevier

The U(Pb)-Pb age of zircon is commonly used to represent the crystallization age for igneous rocks due to its high closure temperature and robust resistance to impact disturbance. However, no zircon crystallization age has yet been reported for Chang’e-5 (CE-5) basalt due to their limited occurrence in mare basalt. In this study, rare zircon grains from CE-5 lunar samples were investigated by the in-situ Pb isotopic analysis, and a precise zircon crystallization age of 2036 ± 19 Ma was determined from Pb-Pb isochron. This is hitherto the youngest reported crystallization age of lunar zircon, similar to the ages of CE-5 lunar basalts obtained by zirconium (Zr)-bearing minerals such as baddeleyite, tranquillityite, and zirconolite. Petrographic evidence and rare-earth element geochemistry indicate that zircon in the CE-5 lunar basalts were formed by the reaction of early-formed baddeleyite with SiO2 melt within the latest residue of extreme fractionation of a non-KREEP (an acronym for potassium, REE, and phosphorus) basaltic magma. In contrast to the prevailing view that lunar zircon have formed in late-stage enriched melts resulting from extensive fractional crystallization of the Lunar Magma Ocean, this study shows that zircon could be derived from extreme fractionation of non-KREEP basaltic magma unrelated to Lunar Magma Ocean.

^1,2Akaogi, Masaki, ¹Miyazaki, Natsuki,¹Tajima, Taisuke,¹Kojitani, Hiroshi
Physics and Chemistry of Minerals 50, 23 Link to Article [DOI 10.1007/s00269-023-01247-4]
¹Department of Chemistry, Gakushuin University, Mejiro, Toshima-ku, Tokyo, 171-8588, Japan
²Geochemical Research Center, Graduate School of Science, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Ali Ettehadi,¹Mehdi Mokhtari,¹Maksym Chuprin,²Robert C. Anderson,³Gursat Altun,⁴Ezat Heydari
Icarus (in Press) Link to Article[https://doi.org/10.1016/j.icarus.2023.115760]
¹University of Louisiana at Lafayette, Louisiana, USA
²Jet Propulsion Laboratory (JPL), California, USA
³Istanbul Technical University, Istanbul, Turkey
⁴Jackson State University, MS, USA
Copyright Elsevier

The MSL (Mars Science Lab) Curiosity rover has documented the presence of natural fractures at the Gale crater on Mars. Through the utilization of the ChemCam instrument, the chemical composition of the veins on Mars has been analyzed, revealing their mineralogy as calcium sulfate. However, there is limited knowledge regarding the mechanical properties of these veins, which hinders a deeper understanding of their origin. This work aims to characterize the mechanical properties of gypsiferous Triassic Moenkopi mudrocks as the terrestrial rock analog to Mars. The Digital Image Correlation (DIC) technique was used in tandem with the Indirect Tensile Strength test to acquire the required spatial full-field strain maps for characterizing the fracture propagation with complex geometries in addition to the derived mechanical properties. The effect of the primary vein orientation on the exerted load on the load-strain profile, fracture initiation and propagation, and tensile strength was established. The dynamic spatial horizontal, vertical, and shear strains’ progression was distinguished through DIC imaging. The key findings include: (1) Different failure modes were observed in samples with and without calcium sulfate veins, with higher tensile strength perpendicular to lamination; (2) Most samples with veins exhibited reduced tensile strength, except when oriented 90° to the load; (3) Fracture paths were influenced by the orientation angle, with irregular paths at certain angles and more regular paths for centrally located veins; (4) Digital image correlation revealed a fracture process zone before macro-crack initiation and subsequent shear crack propagation; (5) Shear strain accumulation preceded shear crack propagation, with potential initiation of tensile cracks.

^1,2Yoko Kebukawa et al.(>10)
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.14064]
¹Department of Chemistry and Life Science, Yokohama National University, Yokohama, Japan
²Yoko Kebukawa, Department of Chemistry and Life Science, Yokohama National University, 79-5 Tokiwadai, Hodogaya-ku, Yokohama 240-8501, Japan.
Published by arrangement withe John Wiley & Sons

The infrared spectral characteristics of organic-rich acid residues prepared from Ryugu samples returned by the JAXA Hayabusa2 mission generally match those from unheated carbonaceous chondrite meteorites, but the residues from Ryugu are richer in methyl and methylene functional groups and have higher CH2/CH3 ratios. Moreover, two distinct outlier carbonaceous phases are found; one with spectral characteristics of N-H functional groups, likely amides, and a second phase containing less nitrogen. Such infrared characteristics of Ryugu organic matter might indicate the pristine nature of the freshly collected samples and reflect the near-surface chemistry in the parent asteroid.

¹Liam D. Peterson,¹Megan E. Newcombe,²Conel M.O’D. Alexander,²Jianhua Wang,⁴Frieder Klein,^3,5,6David V. Bekaert,^3,5Sune G. Nielsen
Earth and Planetary Science Letters 620, 118341 Link to Article [https://doi.org/10.1016/j.epsl.2023.118341]
¹Department of Geology, University of Maryland, College Park, MD 20740, United States
²Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, United States
³NIRVANA Labs, Woods Hole Oceanographic Institution, Woods Hole, MA 02540, United States
⁴Department of Marine Chemistry and Geochemistry, Woods Hole Oceanographic Institution, Woods Hole, MA 02540, United States
⁵Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02540, United States
⁶Université de Lorraine, CNRS, CRPG, 54000 Nancy, France
Copyright Elsevier

Aubrites and enstatite chondrites (ECs) are isotopically similar to the Earth and therefore may resemble the primary materials that accreted to form our planet. Recent bulk H elemental and isotopic analyses of ECs and the Norton County aubrite suggest that enstatite-rich materials are H-rich and may represent a significant source of terrestrial water, with measured values of 3000±2000 μg/g H2O and 5300±900 μg/g H2O in the bulk and enstatite fractions of Norton County (Piani et al., Science, 2020). Here, we present a detailed investigation of in situ H2O concentrations in enstatite, diopside, forsterite, and plagioclase from a suite of main group aubrites, including Norton County, and Shallowater. We find that enstatite (4±2 μg/g H2O), diopside (4.8±0.5 μg/g H2O), and forsterite (5±3 μg/g H2O) have similar H2O concentrations, and all are significantly lower than plagioclase (24±3 μg/g H2O). We combine our in situ analyses of H2O contents with equilibrium partition coefficients and bulk mineralogies to estimate the bulk H2O content of our samples. We compare these first order estimates with bulk volatile analyses conducted using sample pyrolysis and find that the previous bulk H2O analyses of aubrites predominantly reflect terrestrial contamination and alteration. If our conclusion that the reported bulk H2O analyses of Norton County primarily reflect terrestrial contamination and alteration extends to bulk analyses of ECs, then EC-like material may not be a significant source of terrestrial water. Our results support the hypothesis that thermal metamorphism, melting, and differentiation leads to efficient desiccation of planetesimals relative to chondrites, and that differentiated planetesimals contributed, at most, trace amounts to Earth’s water budget.

¹Chandran, Saranya R.,¹James S.,¹Aswathi J.,¹Padmakumar, Devika,¹Marjan, T. Sadeeda,¹Kumar, R.B. Binoj,^2,4Chavan, Anil,²Bhandari, Subhash ^1,3Sajinkumar K.S.
Earth-Science Reviews 243, 104508 Link to Article [DOI 10.1016/j.earscirev.2023.104508]
¹Department of Geology, University of Kerala, Thiruvananthapuram, 695581, India
²Department of Earth and Environmental Science, K.S.K.V. Kachchh University, Bhuj-Kachchh, 370001, India
³Department of Geological and Mining Engineering and Sciences, Michigan Technological University, Houghton, 49931, MI, United States
⁴Physical Research Laboratory, Ahmedabad, 380009, India

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Wang, Jin,¹Li , Detian,²Liu, Kun,¹Yan, Chunjie,²Qing, Gang,¹Wang, Chunyong
Zhenkong Kexue yu Jishu Xuebao/Journal of Vacuum Science and Technology 43, 271 – 289 Link to Article [DOI 10.13922/j.cnki.cjvst.202210018]
¹Science and Technology on Vacuum Technology and Physics Laboratory, Lanzhou Institute of Physics, Lanzhou, 730000, China
²School of Mechanical Engineering and Automation, Northeastern University, Shenyang, 110819, China

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Liu, Xianfeng et al. (>10)
Space Science Reviews 219, 43 Link to Article [DOI 10.1007/s11214-023-00987-7]
¹Key Laboratory of Space Active Opto-electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences (CAS), Shanghai, 200083, China
²Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, CAS, Beijing, 100101, China

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Wang, Xu,¹Zhang, Guozhuo,¹Li, Angze,¹Wang, Yun,¹Cui, Han,¹Zhao, Weiqian,¹Qiu, Lirong
Spectrochimica Acta -Part B Atomic Spectroscopy 207, 106759 Link to Article [DOI 10.1016/j.sab.2023.106759]
¹MIIT Key Laboratory of Complex-filed Intelligent Exploration, School of Optics and Photonics, Beijing Institute of Technology, Beijing, 100081, China

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Amanda C. Stadermann,¹Jessica J. Barnes,³Timmons M. Erickson,²Tabb C. Prissel,⁴Zachary D. Michels
Journal of Geophysical Research (Planets) (in Press) Open Access Link to Article [https://doi.org/10.1029/2022JE007728]
¹Lunar and Planetary Laboratory, University of Arizona, 1629 E University Blvd, Tucson, AZ, 85721 USA
²Astromaterials Research and Exploration Science at NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX, 77058 USA
³Jacobs JETS at NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX, 77058 USA
⁴Department of Geosciences, University of Arizona, 1040 E 4th St, Tucson, AZ, 85721 USA
Published by arrangement with John Wiley & Sons

The magnesian suite (Mg-suite) of rocks record some of the earliest intrusive magmatism on the Moon. Studies of these Mg-suite rocks find they are plutonic or hypabyssal, formed typically kilometers under the lunar surface. Several models exist to explain the formation and evolution of the Mg-suite but distinguishing between hypotheses can be difficult given limited sample availability. The global extent of Mg-suite magmatism remains in debate and is key to constraining models of early secondary crust building. In this study, we present magnesian clasts within Apollo impact melt rock 68815. These clasts contain olivine, plagioclase, with minor amounts of Mg-Al-spinel and pyroxene similar to spinel troctolites of the Mg-suite, but they lack plutonic textures. We provide evidence that some of the clasts may be of extrusive volcanic origin akin to terrestrial komatiites while others might represent crystalline impact melts. There exists a large breadth of evidence for Mg-suite intrusives, whereas here we present possible evidence of Mg-rich volcanic counterparts. If valid, this would broaden the known diversity of lunar volcanism during the initial stages of secondary crust building. We anticipate this finding to provide a greater constraint onto models of Mg-suite ascent and emplacement, which only currently consider intrusive magmatism, as well as a renewed motivation to examine impact melt breccias for rare and understudied lithologies. Future trace element studies or radiometric dating could be used to further interrogate the connections of these clasts to the Mg-suite.