^1,7,8Wen Yu et al. (>10)
Earth and Planetary Science Letters 655, 119263 Link to Article [https://doi.org/10.1016/j.epsl.2025.119263]
¹Center for Lunar and Planetary Sciences, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China
⁷CAS center for Excellence in Comparative Planetology, Hefei 230026, China
⁸Key Laboratory of Space Manufacturing Technology, Chinese Academy of Sciences, Beijing, 100094, China
Copyright Elsevier

The image of a bone-dry surface in the Moon’s non-polar regions impinged by the Apollo missions was changed by the detection of widespread absorption near 3 µm in 2009, interpreted as a signature of hydration. However, debates persist on the relative contribution of molecular water (H2O) and other hydroxyl (OH) compounds to this hydration feature, as well as the cause of the potential temperature-dependence of the OH/H2O abundance. Resolving these debates will help to estimate the inventory of water on the Moon, a crucial resource for future space explorations. In this study, we measured the abundance and isotope composition of hydrogen within the outermost micron of Chang’e-5 soil grains, collected from the lunar surface and from a depth of 1 m. These measurements, combined with our laboratory simulation experiments, demonstrate that solar-wind-induced OH can be thermally retained in lunar regolith, with an abundance of approximately 48–95 ppm H2O equivalent. This abundance exhibits small latitude dependence and no diurnal variation. By integrating our results with published remote sensing data, we propose that a high amount of molecular water (∼360 ± 200 ppm H2O) exists in the subsurface layer of the Moon’s non-polar regions. The migration of this H2O accounts for the observed latitude and diurnal variations in 3 µm band intensity. The inventory of OH and H2O proposed in this study reconciles the seemingly conflicting observations from various instruments, including infrared/ultraviolet spectroscopies and the Neutral Mass Spectrometer (NMS). Our interpretation of the distribution and dynamics of lunar hydration offers new insights for future lunar research and space

¹ Tiwari,¹Gaurav Joshi,¹Pradyut Phukon,¹Amar Agarwal,²Mamilla Venkateshwarlu
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.14323]
¹Applied Structural Geology Lab, Department of Earth Sciences, Indian Institute of Technology Kanpur, Kanpur, Uttar Pradesh, India
²CSIR-National Geophysical Research Institute, Hyderabad, Telangana, India
Published by arrangement with John Wiley & Sons

At the Dhala impact structure, the monomict breccia and the impact melt rock outcrops are present in proximity. Generally, these impactite lithologies are formed by different mechanisms and in different parts of the crater. The emplacement setting of impact melt rocks at Dhala has been well studied. Therefore, we studied the emplacement of monomict breccia using field, microscopic, and magnetic fabric investigations. Our results show that the intensities of the rock magnetic parameters in monomict breccia are comparable with the unshocked target granitoid at Dhala. Thus, the magnetic fabrics developed during pre-impact processes and were not altered due to impact. The absence of the reorientation of magnetic fabrics indicates that the peak shock pressures were below 0.5 GPa. Such shock pressures typically exist near the crater wall/floor or outside the crater. Moreover, there is no local variation in the orientations of magnetic fabrics at different locations in the same outcrop. Thus, the monomict breccia was not displaced from their pre-impact position. Based on the shock barometry and absence of displacement, we propose that the present-day annular outcrops of monomict breccia are located just outside the final crater. Furthermore, the monomict breccia annular outcrop ring has an internal diameter of ~4.5 km and is juxtaposed with impact melt rocks, which formed within the crater (previous studies). We, thus, suggest that the present-day crater diameter is ~4.5 km.

¹Taddei, Alice,²Holtstam, Dan,^1,3Bindi, Luca
Mineralogical Magazine (in Press) Link to Article [DOI 10.1180/mgm.2024.78]
¹Dipartimento di Scienze della Terra, Università degli Studi di Firenze, via La Pira 4, Firenze, I-50121, Italy
²Department of Geosciences, Swedish Museum of Natural History, Box 50007, Stockholm, SE-10405, Sweden
³CNR, Istituto di Geoscienze e Georisorse, sezione di Firenze, via La Pira 4, Firenze, I-50121, Italy

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

¹Galuskin, Evgeny V.,¹Galuskina, Irina O.,³Vapnik, Yevgeny,⁴Zieliński, Grzegorz
Mineralogical Magazine (in Press) Open Access Link to Article [DOI 10.1180/mgm.2025.3]
¹Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia, Będzińska 60, Sosnowiec, 41-200, Poland
²Faculty of Science and Technology, University of Silesia, 75. Pułku Piechoty 1, Chorzów, 41-500, Poland
³Department of Geological and Environmental Sciences, Ben-Gurion University of the Negev, P.O.B. 653, Beer-Sheva, 84105, Israel
⁴Polish Geological Institute, National Research Institute, Rakowiecka 4, Warsaw, 00-975, Poland

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

^1,2Liu, Shuyun,^1,2Zhao, Haifeng,¹Yuan, Zihao,^1,2Xiao, Liping,^1,2Shen, Chengcheng,^1,2Wan, Xue,^3,4Tang, Xuhai,²Zhang, Lu
Aerospace 12, 26 Open Access Link to Article [DOI 10.3390/aerospace12010026]
¹University of Chinese Academy of Sciences, Beijing, 100039, China
²Technology and Engineering Center for Space Utilization, Chinese Academy of Sciences, Beijing, 100094, China
³School of Civil Engineering, Wuhan University, Wuhan, 430072, China
⁴Wuhan University Shenzhen Research Institute, Shenzhen, 518057, China

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

^1,,3Chernonozhkin S.M.,^4,5Pittarello L.,⁶Hublet G.,⁷Weyer S.,⁷Horn I.,⁸Claeys P.,⁶Debaille V.,¹Vanhaecke F.,⁸Goderis S.
Geochemical Research Letters 33, 38-43 Open Access Link to Article [DOI 10.7185/geochemlet.2501]
¹Atomic & Mass Spectrometry – A&MS Research Unit, Department of Chemistry, Ghent University, Campus Sterre, Krijgslaan, 281 – S12, Ghent, B-9000, Belgium
²Research Group – Isotope Ratio Analysis, Montanuniversität Leoben, Franz Josef-Straße 18, Leoben, 8700, Austria
³Geological Survey of Finland, P.O. Box 96, Espoo, 02151, Finland
⁴Naturhistorisches Museum Wien – NHMW, Mineralogisch-Petrographische Abteilung, Burgring 7, Vienna, 1010, Austria
⁵University of Vienna, Department of Lithospheric Research, Josef-Holaubek-Platz 2, Vienna, 1090, Austria
⁶Laboratoire G-Time, Université Libre de Bruxelles, 50, Av. F.D. Roosevelt CP 160/02, Brussels, B-1050, Belgium
⁷Institute of Earth System Sciences, Section Mineralogy, Leibniz Universität Hannover, Callinstr. 3, Hannover, 30167, Germany
⁸Archaeology, Environmental Changes, and Geo-Chemistry (AMGC), Vrije Universiteit Brussel, Pleinlaan 2, Brussels, 1050, Belgium

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

^1,2,3Gao, Fang,^1,2Liu, Bin,^1,2Zhou, Qin,^1,2Li, Chun-Lai
Research in Astronomy and Astrophysics 25, 015005 Link to Article [DOI
10.1088/1674-4527/ad95d8]
¹Key Laboratory of Lunar and Deep Space Exploration, Chinese Academy of Sciences, Beijing, 100012, China
²National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China
³University of Chinese Academy of Sciences, Beijing, 100049, China

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

¹Iizuka, Tsuyoshi,^2,3Hibiya, Yuki,¹Yoshihara, Satoshi,⁴Hayakawa, Takehito
Astrophysical Journal Letters 979, L29 Open Access Link to Article [DOI 10.3847/2041-8213/ada554]
¹Department of Earth and Planetary Science, The University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo, 113-0033, Japan
²Research Center for Advanced Science and Technology, The University of Tokyo, Komaba 4-6-1, Meguro, Tokyo, 153-8904, Japan
³Submarine Resources Research Center, Japan Agency for Marine-Earth Science and Technology, Kanagawa, 237-0061, Japan
⁴Kansai Institute for Photon Science, National Institutes for Quantum Science and Technology, Umemidai 8-1-7, Kizugawa, Kyoto, 619-0215, Japan

The radioactive decay of short-lived 26Al-26Mg has been used to estimate the timescales over which 26Al was produced in a nearby star and the protosolar disk evolved. The chronology commonly assumes that 26Al was uniformly distributed in the protosolar disk; however, this assumption is challenged by the discordance between the timescales defined by the Al-Mg and assumption-free Pb-Pb chronometers. We find that the 26Al heterogeneity is correlated with the nucleosynthetic stable Ti isotope variation, which can be ascribed to the nonuniform distribution of ejecta from a core-collapse supernova in the disk. We use the Al-Ti isotope correlation to calibrate variable 26Al abundances in Al-Mg dating of early solar system processes. The calibrated Al-Mg chronometer indicates a ≥1 Myr gap between parent body accretion ages of carbonaceous and noncarbonaceous chondrites. We further use the Al-Ti isotope correlation to constrain the timing and location of the supernova explosion, indicating that the explosion occurred at 20-30 pc from the protosolar cloud, 0.94 +0.25/-0.21 Myr before the formation of the oldest solar system solids. Our results imply that the Sun was born in association with a ∼25 Mʘ star.

¹Takaaki Noguchi,^2,3Takahito Tominaga,^2,4Minako Takase,⁵Akira Yamaguchi,⁵Naoya Imae
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.14324]
¹Division of Earth and Planetary Science, Kyoto University, Kyoto, Japan
²Department of Earth and Planetary Science, Kyushu University, Fukuoka, Japan
³Kai Industries Co. Ltd., Gifu, Japan
⁴Fukuoka City Science Museum, Fukuoka, Japan
⁵National Institute of Polar Research, Japan, Tokyo, Japan
Published by arrangement with John Wiley & Sons

Over a period of 16 years, we collected Antarctic micrometeorites (AMMs) preserved in 1-t snow samples from the surface to a depth of ~10–15 cm near Dome Fuji Station, Antarctica. A total of 1025 AMMs were identified: 843 unmelted AMMs, 51 scoriaceous ones, and 131 cosmic spherules. Their average sizes were 40, 64, and 40 μm, respectively. The accretion rate of AMMs was inferred to be (3.3 ± 1.8) × 103 t year−1, based on the snow accumulation rate near Dome Fuji Station. We compared the Dome Fuji collection (DFC) with our previous Tottuki #5 collection (T5C) recovered from blue ice in 2000. Regardless of the collection methods, the full range size distributions of AMMs were well fitted by lognormal functions. In 2019 and 2020, we applied a freeze-drying (FD) system to collect AMMs. We identified 21 AMMs from 17 kg of surface snow. Both GEMS (glass with embedded metal and sulfide)-rich chondritic porous (CP) AMMs and hydrated fine-grained (H f-g) AMMs were identified. No detectable mineralogical differences were observed between a CP AMM from the DFC-FD and one from the DFC, suggesting that ~6 h of exposure to cold water (<8.7°C) did not affect the mineralogy of CP AMMs.

^1,2N.G. Rudraswami, ^1,2V.P. Singh, ¹M. Pandey
Chemical Geology 677, 122628 Link to Article [https://doi.org/10.1016/j.chemgeo.2025.122628]
¹National Institute of Oceanography (Council of Scientific and Industrial Research), Dona Paula, Goa 403004, India
²Academy of Scientific and Innovative Research (AcSIR), Ghaziabad 201002, India

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