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

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^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

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^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

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^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

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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

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^1,3Hyung, Eugenia,^2,3Cherston, Juliana,^1,3Jacobsen, Stein B.,^2,3Loeb, Abraham Avi
Chemical Geology 677, 122627 Link to Article [DOI 10.1016/j.chemgeo.2025.122627]
¹Dept. of Earth and Planet. Sci., Harvard Univ., Cambridge, 02138, MA, United States
²Dept. of Astronomy, Harvard Univ., Cambridge, 02138, MA, United States
³Interstellar Expedition of the Galileo Project, Cambridge, 02138, MA, United States

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^1,2Dettori, Riccardo^1,2Goldman, Nir
Journal of Physical Chemistry A, 129 583-595 Link to Article [DOI 10.1021/acs.jpca.4c05881]
¹Physical and Life Sciences Directorate, Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, 94550, CA, United States
²Department of Physics, University of Cagliari, CA, Monserrato, 09042, Italy
³Department of Chemical Engineering, University of California, Davis, 95616, CA, United States

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¹Elmer J.W.,¹Bellino J.S.
Acta Astronautica 229, 578-590 Link to Article [DOI 10.1016/j.actaastro.2025.01.018]
¹Materials Engineering Division, Lawrence Livermore National Laboratory, Livermore, CA, United States

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