^1,2Soukaina Arif, ^1,2Hasnaa Chennaoui Aoudjehane, ³Audrey Bouvier
Minerals, 16, 44
Open Access Link to Article [DOI: 10.3390/min16010044]
¹GeoPen Laboratory, Faculty of Science Ain Chock, Hassan II University of Casablanca, Km 8 Route d’El Jadida, Casablanca 20150, Morocco
²ATTARIK Foundation for Meteoritics and Planetary Science, Casablanca 20150, Morocco
³Bayerisches Geo-Institut, Universitätsstraße 30, 95447 Bayreuth, Germany

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¹P. N. Simon, ¹P. Vernazza, ²M. Marsset, ³M. Brož, ⁴R. P. Binzel, ⁴F. DeMeo, ⁵C. A. Thomas, ¹L. Jorda
Astronomy & Astrophysics, 714, A514
Open Access Link to Article [DOI: 10.1051/0004-6361/202661440]
¹Aix-Marseille University, CNRS, CNES, LAM, Institut Origines, 38 rue Frederic Joliot Curie, 13388 Marseille, France
²European Southern Observatory (ESO), Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
³Charles University, Faculty of Mathematics and Physics, Institute of Astronomy, V Holešovičkách 2, 18200, Czech Republic
⁴Department of Earth, Atmospheric and Planetary Sciences, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
⁵Department of Astronomy and Planetary Science, Northern Arizona University PO Box 6010, Flagstaff, AZ 86011, USA

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¹C. Lantz et al. (>10)
Astronomy & Astrophysics, 713, L21
Open Access Link to Article [DOI: 10.1051/0004-6361/202662059]
¹Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, 91405 Orsay Cedex, France

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^1,2Kairui Tai et al. (>10)
Astronomy & Astrophysics, 713, A231
Open Access Link to Article [DOI: 10.1051/0004-6361/202556910]
¹Research Center for Planetary Science, College of Earth and Planetary Sciences, Chengdu University of Technology, Chengdu 610059, PR China
²Lunar and Planetary Sciences Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, PR China

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¹Eddy Abdo et al. (>10)
Astronomy & Astrophysics, 713, A156
Open Access Link to Article [DOI: 10.1051/0004-6361/202659972]
¹Institut des Sciences Moléculaires d’Orsay (ISMO), UMR8214, CNRS, Université Paris-Saclay, 91405 Orsay, France

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^1,2,3Sandipan P. D. Borthakur, ^4,3Mihkel Kama, ¹Luca Fossati, ³Colin P. Folsom, ³Anna Aret, ^1,2Christiane Helling
Astronomy & Astrophysics, 713, L13
Open Access Link to Article [DOI: 10.1051/0004-6361/202661500]
¹Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
²Institute for Theoretical and Computational Physics, Graz University of Technology, Petersgasse 16, 8010 Graz, Austria
³Tartu Observatory, University of Tartu, Observatooriumi 1, Tõravere, 61602, Estonia
⁴Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

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¹Scott A. Eckley (>10)
Meteoritics & Planetary Science, (in Press), 1–26
Open Source Link to Article [DOI: 10.1111/maps.70205]

¹Amentum, JETS 2, NASA Johnson Space Center, Houston, Texas, USA
Published by arrangement with John Wiley & Sons

The OSIRIS-REx mission collected a 121.6 g regolith sample from the surface of asteroid Bennu. Preliminary examination (PE) was conducted jointly by JSC Curation and the OSIRIS-REx Sample Analysis Team. To enable advanced, non-destructive characterization during PE, 59 centimeter-scale stones were individually scanned using X-ray computed tomography (XCT) inside custom-built containers to preserve their pristine condition. The XCT data provide three-dimensional petrographic context that supports PE, sample processing and allocation, and subsequent scientific investigations. We analyzed 14.46% ± 0.03% (17.585 ± 0.038 g) of the total returned sample mass and document extensive lithologic diversity within the collection. The samples are divided into two primary groups, monolithic and clastic, which are further subdivided into nine lithological categories. Using XCT-derived volumes combined with measured masses, we find that the monolithic group is denser than the clastic group, and some monolithic lithologies exhibit statistically higher average densities, likely reflecting differences in composition and/or internal structure. Shape, quantified using orthogonal caliper measurements and Sneed & Folk and Zingg classifications, does not systematically correspond to lithology. The monolithic-dark-veined lithology is an exception, exhibiting consistently flat, bladed shapes. Correspondence between stone morphology, defined as hummocky, angular, or mottled, and lithology varies. Using X-ray attenuation contrast in conjunction with prior petrographic and compositional studies, we identify veins, large carbonates, candidate chondrules, coarse-grained pyrrhotite assemblages, ~25 μm long highly-X-ray-attenuating phases that possibly contain platinum group elements and surface micro-impact craters. These results provide a three-dimensional petrographic framework for continued characterization of the returned sample and for deciphering Bennu’s origin and geological history.

¹Birgit Schulz, ¹Christian Vollmer, ²Peter Hoppe, ^2,3Jan Leitner, ⁴Lindsay P. Keller
Meteoritics & Planetary Science, (in Press), 1–15
Open Source Link to Article [DOI: 10.1111/maps.70257]

¹Institut für Mineralogie, Universität Münster, Münster, Germany
²Max-Planck-Institut für Chemie, Mainz, Germany
³Institut für Geowissenschaften, Ruprecht-Karls-Universität Heidelberg, Heidelberg, Germany
⁴XI3, Astromaterials Research and Exploration Science (ARES) Division, NASA Johnson Space Center, Houston, Texas, USA
Published by arrangement with John Wiley & Sons

Eight anhydrous interplanetary dust particles (IDPs) were analyzed for their oxygenisotopic compositions and mineralogy. They show oxygen isotopic compositions from 16O-rich to16O-poor, due to mixing of different reservoirs inherited from the protosolar molecular cloud andthe early solar nebula. Glass with embedded metal and sulfide (GEMS) in anhydrous IDPsrecord a variety of formation environments in which they adopted oxygen isotopic compositionof surrounding gas, because amorphous silicates exchange isotopes with gaseous species moreeffectively than crystalline materials due to their open framework. Equilibrated aggregates (EAs)form from GEMS via secondary processes that involve recrystallization and have similarchemical and isotopic heterogeneity as GEMS. A common feature of most anhydrous IDPs is aslight enrichment either in 17O or, rarer, in 18O relative to a slope-1 line on which primitivemeteorites and their components plot. Possible explanations might be organic matter enriched inheavy oxygen. Although some of the investigated IDPs show hints of atmospheric entry heating,oxygen isotopic compositions of the IDPs are not shifted toward the terrestrial fractionation line(TFL), as seen for larger micrometeorites and cosmic spherules. Thus, we conclude thatanhydrous IDPs preserve primordial oxygen isotopic compositions of early solar systemreservoirs.