^1,2,3Daviau K.,¹Fischer R.A.,¹Brennan M.C.,¹Dong J.,¹Sure T.-A.,⁴Couper S.,⁵Meng Y.,⁶Prakapenka V.B.
Journal of Geophysical Research: Solid Earth 126, e2020JB020074 Link to Article [DOI
10.1029/2020JB020074]
¹Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, United States
²Now at School of Science, University of Waikato, Tauranga, New Zealand
³Now at Toi-Ohomai Institute of Technology, Tauranga, New Zealand
⁴Department of Geology and Geophysics, University of Utah, Salt Lake City, UT, United States
⁵HPCAT, X-Ray Science Division, Argonne National Laboratory, Argonne, IL, United States
⁶Center for Advanced Radiation Sources, University of Chicago, Chicago, IL, United States

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¹Cavosie A.J.,²Biren M.B.,²Hodges K.V.,^cWartho J.-A.,⁴Horton Jr. J.W.,⁵Koeberl C.
Geology 49, 201-205 Link to Article [DOI 10.1130/G47860.1]
¹Space Science and Technology Centre, Institute for Geoscience Research, School of Earth and Planetary Science, Curtin University, Perth, 6102, Western Australia, Australia
²School of Earth and Space Exploration, Arizona State University, Tempe, 85287, Arizona, United States
³GEOMAR Helmholtz Centre for Ocean Research Kiel, Kiel, 24148, Germany
⁴U.S. Geological Survey, 926A National Center, Reston, 20192, Virginia, United States
⁵Department of Lithospheric Research, University of Vienna, Althanstrasse 14, Vienna, A-1090, Austria

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¹Nakada R.,²Tanabe G.,^2,3Kajitani I.,^3,4Usui T.,²Shidare M.,²Yokoyama T.
Minerals 11, 176 Link to Article [DOI 10.3390/min11020176]
¹Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), 200 Monobe, Kochi, Nankoku, 783-8501, Japan
²Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo, 152-8551, Japan
³Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Kanagawa, Sagamihara, 252-5210, Japan
⁴Earth-Life Science Institute, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo, 152-8551, Japan

¹Chernonozhkin S.M.,²McKibbin S.J.,³Goderis S.,¹Van Malderen S.J.M.,³Claeys P.,¹Vanhaecke F.
Chemical Geology 562, 119996 Link to Article [DOI 10.1016/j.chemgeo.2020.119996]
¹Ghent University, Department of Chemistry, Atomic & Mass Spectrometry – A&MS Research Unit, Campus Sterre, Krijgslaan, 281 – S12, Ghent, 9000, Belgium
²Geowissenschaftliches Zentrum, Abteilung Isotopengeologie, Georg-August-Universität Göttingen, Goldschmidtstraße 1, Göttingen, 37073, Germany
³Vrije Universiteit Brussel, Analytical, Environmental, and Geo-Chemistry, Pleinlaan 2, Brussels, 1050, Belgium

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^1,2Pourkhorsandi H.,^1,3Debaille V.a,Armytage R.M.G.,^1,4van Ginneken M.,²Rochette P.,²Gattacceca J.
Chemical Geology 562, 120056 Link to Article [DOI 10.1016/j.chemgeo.2020.120056]
¹Laboratoire G-Time, Université Libre de Bruxelles, 160/02, 50, Av. F.D. Roosevelt, Brussels, 1050, Belgium
²Aix-Marseille Univ, CNRS, IRD, INRAE, CEREGE, Aix-en-Provence, France
³Jacobs/JETS, NASA Johnson Space Center, 2101 NASA Parkway, Mailcode XI3, Houston, 77058, United States
⁴Royal Belgium Institute of Natural Sciences, rue Vautier 29, Bruxelles, B-1000, Belgium

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¹Garcia-Florentino C.,¹Torre-Fdez I.,¹Ruiz-Galende P.,¹Aramendia J.,¹Castro K.,¹Arana G.,²Maguregui M.,¹Ortiz de Vallejuelo S.F.,¹Madariaga J.M.
Talanta 224, 121863 Link to Article [DOI 10.1016/j.talanta.2020.121863]
¹Department of Analytical Chemistry, Faculty of Science and Technology, University of the Basque Country UPV/EHU, Barrio Sarriena S/n, Leioa, 48940, Spain
²Department of Analytical Chemistry, Faculty of Pharmacy, University of the Basque Country UPV/EHU, P.O. Box 450, Vitoria-Gasteiz, 01080, Spain

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^1,2,3,4Zhang C.,^1,3Miao B.,⁵He H.,^1,3Chen H.,⁵Ranjith P.M.,⁴Xie Q.
Minerals 11, 279 Link to Article [DOI 10.3390/min11030279]
¹Institution of Meteorites and Planetary Materials Research, Guilin University of Technology, Guilin, 541006, China
²Key Laboratory of Lunar and Deep Space Exploration, Chinese Academy of Sciences, Beijing, 100029, China
³Guangxi Key Laboratory of Hidden Metallic Ore Deposits Exploration, Guilin University of Technology, Guilin, 541006, China
⁴College of Environmental Science and Engineering, Guilin University of Technology, Guilin, 541006, China
⁵Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, 100029, China

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¹Vincenzo Stagno,²Luca Bindi,⁴Sota Takagi,⁴Atsushi Kyono
Progress in Earth and Planetary Science 8, 27 Link to Article [DOI
https://doi.org/10.1186/s40645-021-00421-y%5D
¹Dipartimento di Scienze della Terra, Università La Sapienza, P.zle Aldo Moro 5, I-00185, Rome, Italy
²Dipartimento di Scienze della Terra, Università di Firenze, Via La Pira 4, I-50121, Florence, Italy
³Institute of Materials Structure Science, High Energy Accelerator Research Organization (KEK), Ibaraki, Japan
⁴Division of Earth Evolution Sciences, Graduate School of Life and Environmental Sciences, University of Tsukuba, Ibaraki, Japan

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^1,2Feng Yin,³Thomas G. Sharp,²Ming Chen
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13702]
¹Department of Geology, Hunan University of Science and Technology, Xiangtan, 411201 China
²Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, 510640 China
³School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, 85287 USA
Published by arrangement with John Wiley & Sons

Coesite embedded in silica glass in suevite from the Xiuyan crater has been studied by scanning and transmission electron microscopy to better understand the mechanisms at formation of coesite. Coesite grains in this study mainly occur as vein-like aggregates (10–40 μm in width) and irregular aggregates (IAs; <40 μm in size). Both aggregate types are composed of subhedral to anhedral coesite crystals with random orientations. Most of the crystals are 100–1000 nm in size, and some display twinning. The shape, twinning, and random orientation of coesite crystals suggest rapid crystallization in amorphous silica that became supercooled. The center of vein-like aggregates crystallized from localized silica melt within diaplectic silica glass, whereas the rim of vein-like aggregates and IAs crystallized from diaplectic silica glass. The size and amount of coesite crystals in the vein-like aggregate vary greatly from the rim to the center of such veins. Microstructures suggest that the crystals nucleated heterogeneously at the outer rim of the vein and nucleated homogeneously within the vein. IAs do not show any changes in size and amount of coesite crystals from the rim to core of such aggregates. Coesite crystals in IAs primarily nucleate heterogeneously in diaplectic silica glass. It can be concluded that vein-like coesite aggregates are mainly formed by crystallization from silica melt, and irregular coesite aggregates should be formed by solid-state transformation of diaplectic silica glass.

¹Bradley T. De Gregorio,²Jessica Opsahl-Ong,³Lysa Chizmadia,¹Todd H. Brintlinger,⁴Andrew J. Westphal,¹Rhonda M. Stroud
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13655]
¹Materials Science and Technology Division, U.S. Naval Research Laboratory, Washington, D.C., 20375 USA
²American Society for Engineering Education, Science & Engineering Apprenticeship Program, Washington, D.C., 20036 USA
³Department of Geology and Physics, Georgia Southwestern State University, Americus, Georgia, 31709 USA
⁴Space Sciences Laboratory, University of California Berkeley, Berkeley, California, 94720 USA
Published by arrangement with John Wiley & Sons

The NASA Stardust Interstellar Dust collection provides our current best sample set for direct laboratory analysis of dust grains from the contemporary interstellar dust stream. While a handful of likely interstellar dust grains were identified within the silica aerogel collection media, interstellar dust also impacted Al foils covering the collector frame. Locating these rare impacts requires labor-intensive collection and examination of tens of thousands of high-resolution SEM images. Here, we implement a Python-based algorithm to dramatically reduce the human time investment needed to locate impact craters. The algorithm employs a circular Hough transform to identify circular features in the foil images, followed by several tests to detect characteristic morphological features of impact craters—a dark center and a bright rim, with inclusion of multi-core processing capabilities to significantly increase processing speed. For most data sets, the code produced a pool of potential crater candidates in 1–5% of the input images, producing a more manageable subset of images for a human expert to review. We used this code to locate 31 impact craters across 12 Stardust interstellar foils, 25 of which were located on three adjacent foils, I1008W,1, I1009N,1, and I1020W,1. Many impacts on these foils formed shallow, oblique craters, with residue compositions consistent with solar cell glass and orientations consistent with debris ejected from the spacecraft solar cells. The code can be integrated into future searches for Stardust interstellar grain impacts and can be implemented as a general utility for dust impact studies on spacecraft materials.