^1,2,3Yash Srivastava, ²James M. D. Day, ⁴Akira Yamaguchi, ¹Amit Basu Sarbadhikari
Communications Earth & Environment (in Press)
Open Access Link to Article [DOI: 10.1038/s43247-025-03046-x]
¹Physical Research Laboratory, Ahmedabad, India
²Scripps Isotope Geochemistry Laboratory, Scripps Institution of Oceanography, University of California San Diego, La Jolla, CA, USA
³Indian Institute of Technology Gandhinagar, Gandhinagar, Gujarat, India
⁴National Institute of Polar Research (NIPR), 10-3 Midori-cho, Tachikawa, Tokyo, Japan

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¹Gaurav Joshi, ¹Satyendra Kumar, ¹Anuja Sreejayan, ²Satadru Bhattacharya, ³Mamilla Venkateshwarlu, ⁴Dewashish Upadhyay, ¹Amar Agarwal
Geoheritage (in Press) Link to Article [DOI: 10.1007/s12371-026-01476-3]
¹Applied Structural Geology Group, Department of Earth Sciences, Indian Institute of Technology Kanpur, Uttar Pradesh, Kanpur, 208016, India
²Planetary Sciences Division, Space Applications Centre, Ahmedabad, 380 015, India
³CSIR-National Geophysical Research Institute, Telangana, Hyderabad, 500007, India
⁴Department of Geology and Geophysics, Indian Institute of Technology, Kharagpur, 721302, India

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¹D. S. Grewal, ²N. X. Nie, ³B. Luais, ²Z. J. Zhang, ³Q. Ahmad, ⁴A. Vazquez Ochoa, ⁴P. Ni
Geochemical Perspectives Letters (in Press)
Open Access Link to Article [DOI: 10.7185/geochemlet.2618]
¹Department of Earth and Planetary Sciences, Yale University, New Haven, 06511, CT, United States
²CAT Lab, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, 02139, MA, United States
³Université de Lorraine, CNRS, CRPG, Nancy, F-54000, France
⁴Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, 90095, CA, United States

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¹Y. Marrocchi, ¹E. Füri, ¹L. Zimmermann, ¹L. Piani
Geochemical Perspectives Letters (in Press)
Open Access Link to Article [DOI: 10.7185/geochemlet.2605]
¹Université de Lorraine, CNRS, CRPG, F-54000 Nancy, France

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^1,2L. A. Lakhmanova, ¹S. I. Demidova, ^1,3V. G. Butvina, ³M. A. Golunova, ^2,4P. Y. Plechov, ³P. G. Bukhtiyarov, ³K. V. Van, ¹G. S. Nikolaeva
Geochemistry International, 64, 1–16
Open Access Link to Article [DOI: 10.1134/S0016702925600786]
¹Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences, Moscow, 119991 Russia
²Moscow State University, Moscow, 119991 Russia
³Korzhinskii Institute of Experimental Mineralogy, Russian Academy of Sciences, Chernogolovka, Moscow oblast, 142432 Russia
⁴Fersman Mineralogical Museum, Moscow, 119071 Russia

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¹Alex M. Ruzicka, ^2,3Jon M. Friedrich, ¹Richard C. Hugo, ⁴Robert J. Macke, ¹Daniel Sheikh, ¹Melinda Hutson
Meteoritics & Planetary Science, (in Press), 1–36
Open Source Link to Article [DOI: 10.1111/maps.70246]

¹Cascadia Meteorite Laboratory, Portland State University, School of Earth, Environment and Society—Earth and Planetary Sciences Academic Area, Portland, Oregon, USA
²Department of Chemistry, Fordham University, Bronx, New York, USA
³Department of Earth and Planetary Sciences, American Museum of Natural History, New York, New York, USA
⁴Vatican Observatory, Vatican City State
Published by arrangement with John Wiley & Sons

Eight different H, L, and LL chondrites with 11 lithologies were studied and showgood evidence for progressive shock effects and compaction. In weakly shocked chondrites(Baszkόwka, Bjurb ¨ole, Saratov, NWA 7298 Lithology A and C), silicates were dominantlyfractured, troilite and metal were more deformed than olivine and fluidized, and estimatedstresses were 4–7 GPa. In strongly shocked chondrites (NWA 7298 Lithology B, NWA11315 Lithology A and B, Alfianello, NWA 8709, NWA 4860), olivine grains display moreplastic deformation than in weakly shocked chondrites and were ultimately recrystallized;troilite, some metal, and some bulk areas were melted; and estimated stresses were >7 GPa.Three settings for lithification are inferred: (A) initial lithification during accretion of warmchondrule aggregates, (B) later lithification in warm, metamorphosing parent bodies thatwere being affected by mainly low-velocity collisions, and (C) final lithification in cool parentbodies after the waning of metamorphic heat that were being affected by higher velocitycollisions. Thus, collisions together with heat of different types (accretionary, metamorphic,and shock-related) were probably the main ways in which unmelted planetesimals werelithified. Impact-fluidized metal and troilite may have acted as important lithification bindingagents even in weak shock events.

^1,2Noemi Mészárosová, ^1,2Roman Skála, ³Mariana Klementová, ³Lukáš Palatinus, ⁴Jozef Veselý, ⁴Petr Harcuba
Meteoritics & Planetary Science, (in Press), 1–14 Link to Article [DOI: 10.1111/maps.70262]

¹Institute of Geochemistry, Mineralogy and Mineral Resources, Faculty of Science, Charles University, Prague 2, Czech Republic
²Institute of Geology of the Czech Academy of Sciences, Prague 6 – Lysolaje, Czech Republic
³Institute of Physics of the Czech Academy of Sciences, Prague 8, Czech Republic
⁴Department of Physics of Materials, Faculty of Mathematics and Physics, Charles University, Prague 2, Czech Republic
Published by arrangement with John Wiley & Sons

A transmission electron microscopy (TEM) study of four troilite grains fromenstatite chondrites (Y-691, Y-791790, Y-86004, A-881314) and two grains from aubrites(Y-793592, Mayo Belwa) addressed their crystal structures and nanoscale mineralogicalrelationships. The crystal structure of troilite in enstatite-rich meteorites is predominantlyconsistent with the space group P62c, except for the FeS phase from Mayo Belwa, whichexhibits a complex modulated structure consistent with a trilling of the modulated NCpyrrhotite superstructure. TEM energy-dispersive X-ray spectroscopy (TEM-EDS) analysesconfirmed the incorporation of chromium and titanium into the troilite crystal structure,even in samples containing nanometer-sized daubr´eelite exsolution lamellae (A-881314, Y-793592). Nanometer-sized inclusions of (Mn,Mg,Fe)S monosulfide solid solution occur introilite in Y-791790. Crystallographic orientation relationships between troilite andassociated sulfide phases (daubr´eelite and keilite) indicate semi-coherent intergrowths at thenanoscale. The absence of nanometer-sized daubr´eelite in Y-86004 and Y-791790 suggestsrapid cooling of the Cr-Fe sulfide solution and quenching of the chemical composition ofthe phase stable above 700°C, consistent with the impact melt origin of these meteorites.Additional weak, diffuse diffractions observed in selected area electron diffraction patternsfor troilites from Y-86004, Y-791790, and Y-793592 are attributed to the development ofvacancy ordering with variable periodicity along the c-axis, corresponding to NC-typesuperstructures. The detailed nature of vacancy ordering and the contributions of Cr andTi substitution to the observed superstructure features remain unresolved and requirecomprehensive structure analysis.