¹Markus Patzek,^2,3Yogita Kadlag,⁴Miriam Rüfenacht,⁵Evelyn Füri,⁶Andreas Pack,¹Addi Bischoff,²Harry Becker,²Robbin Visser,²Timm John,⁴Maria Schönbächler
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.14343]
¹Institut für Planetologie, University of Münster, Münster, Germany
²Freie Universität Berlin, Institut für Geologische Wissenschaften, Berlin, Germany
³Physical Research Laboratory, Ahmedabad, Gujarat, India
⁴Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland
⁵Université de Lorraine, CNRS, CRPG, Nancy, France
⁶Universität Göttingen, Geowissenschaftliches Zentrum, Göttingen, Germany
Published by arrangement with John Wiley & Sons

A multi-element isotope (N, O, Ti, and Cr) study was conducted on C1 and CM-like clasts hosted in achondrites and chondrite breccias to understand the genesis of these chondritic clasts. The mineralogy, O, and N isotopes confirm that CM-like clasts in howardites and polymict eucrites closely resemble CM chondrite-like material. The O and Cr isotope composition of C1 clasts in CR chondrites overlaps with those of CR chondrites, implying either formation in a similar nebular environment or resemblance to local CR material that underwent more extensive in situ alteration. Notably, these clasts are less enriched in 15N than bulk CR chondrites. In contrast, C1 clasts in ureilites are enriched in 15N relative to the Earth’s atmosphere by ~100‰ setting them apart from any other known solar system material. They display elevated 17O and 18O values and lie along the CCAM line. In addition, a C1 clast from an ureilite represents the most 54Cr-enriched and 50Ti-depleted endmember among the carbonaceous chondrites. Altogether, these isotopic characteristics suggest that C1 clasts in ureilites represent material not sampled by any known meteorite group. Overall, this study highlights the presence of primitive, isotopically distinct materials in the early outer solar system, some of which were transported to the inner solar system to the accretion region of the host parent bodies.

^1,2,3Alice Macente,^3,4,5Luke Daly,³Sammy Griffin,^6,7,8Maria Gritsevich,^6,7Jarmo Moilanen,³Josh Franz Einsle,⁹Patrick Trimby,¹⁰Chris Mulcahy,¹⁰Jonathan Moffat,¹¹Alexander M. Ruzicka
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.14344]
¹School of Civil Engineering, University of Leeds, Leeds, UK
²Department of Civil and Environmental Engineering, University of Strathclyde, Glasgow, UK
³School of Geographical and Earth Sciences, University of Glasgow, Glasgow, UK
⁴Australian Centre for Microscopy and Microanalysis, The University of Sydney, Sydney, New South Wales, Australia
⁵Department of Materials, University of Oxford, Oxford, UK
⁶Faculty of Science, University of Helsinki, Helsinki, Finland
⁷Finnish Fireball Network, Helsinki, Finland
⁸Institute of Physics and Technology, Ural Federal University, Ekaterinburg, Russia
⁹Carl Zeiss Limited, Cambourne, UK
¹⁰Oxford Instruments Nanoanalysis, High Wycombe, UK
¹¹Department of Geology and Cascadia Meteorite Laboratory, Portland State University, Portland, Oregon, USA
Published by arrangement with John Wiley & Sons

Combining electron backscatter diffraction (EBSD) with X-ray computed tomography (XCT) offers a comprehensive approach to investigate shock deformation and rock texture in meteorites, yet such integration remains uncommon. In this study, we demonstrate the synergistic potential of XCT and EBSD in revealing deformation metrics, thereby enhancing our understanding of petrofabric strength and shock-induced deformation. Our analysis focuses on the Ozerki (L6, S4/5, W0) meteorite fall, which was instrumentally observed on June 21, 2018, and subsequently recovered by the Ural’s branch of the Russian Fireball Network (UrFU) recovery expedition a few days later. The trajectory analysis conducted by the Finnish Fireball Network facilitated the prompt retrieval of the meteorite. We show that Ozerki is deformed, with a moderate strength foliation fabric defined by metal and sulfide grain shapes. Microstructural analysis using EBSD shows that the parent body was likely still thermally active during this impact event. Our data suggest that these microstructures were likely produced during an impact while the Ozerki’s parent body was still warm.