^1,2Xiande Xie,³Xiangping Gu,⁴Hexiong Yang,²Ming Chen,⁴Kai Li
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13426]
¹Key Laboratory of Mineralogy and Metallogeny, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, 510640 China
²Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou, 510640 China
³School of Geosciences and Info‐Physics, Central South University, Changsha, Hunan, 410083 China
⁴Department of Geosciences, University of Arizona, 1040 E. 4th Street, Tucson, Arizona, 85721‐0077 USA
⁵Institute for Materials Microstructure, Central South University, 410083 Changsha, Hunan, PR China
Published by arrangement with John Wiley & Sons

Wangdaodeite, the shock‐induced lithium niobate–structured polymorph of ilmenite, was found in the Suizhou L6 chondrite. It occurs as small irregular particles (2–20 μm in size) inside or adjacent to the shock melt veins. Wangdaodeite coexists in veins with ringwoodite, majorite, and xieite. The chemical formula of wangdaodeite is FeTiO₃. The empirical formula is: (Fe_0.85Mg_0.10Mn_0.05)_Σ1.00Ti_0.99O₃, which is similar to that of its host ilmenite. The Raman spectra of wangdaodeite display the bands at 174–179, 273–277, 560–567, 738–743 cm⁻¹, which are different to those for ilmenite. TEM images show that ilmenite is composed of polysynthetic‐twinned crystals while wangdaodeite is composed of random‐oriented nanometric domains sized 20–50 nm. Electron diffraction established wangdaodeite to be trigonal with the lithium niobate structure. Cell parameters are: a = 5.13(1) Å, c = 13.78(1) Å; c/a = 2.69; space group R3c; calculated density = 4.72 g cm⁻³. The P–T conditions for formation of wangdaodeite were estimated to be 20–24 GPa and >1200 °C. The mineral name was approved by the Commission on New Minerals, Nomenclature, and Classification of the International Mineralogical Association (IMA 2016‐007). The name is for Daode Wang, Professor at the Guangzhou Institute of Geochemistry, Chinese Academy of Sciences.

¹Gałązka-Friedman, J.,²Woźniak, M.,¹Bogusz, P.,¹Jakubowska, M.,³Karwowski, Ł.,¹Duda, P.
Hyperfine Interactions 241, 20 Link to Article [DOI: 10.1007/s10751-019-1661-0]
¹Faculty of Physics, Warsaw University of Technology, Koszykowa 75, Warsaw, 00-662, Poland
²Faculty of Biology, University of Warsaw, Miecznikowa 1, Warszawa, 02-096, Poland
³Faculty of Earth Sciences, University of Silesia in Katowice, ul. Będzińska 60, Sosnowiec, 41-200, Poland

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^1,2,3,4Nozaki, T. et al. (>10)
Scientific Reports 9, 16111 Link to Article [DOI: 10.1038/s41598-019-52709-1]
¹Submarine Resources Research Center, Research Institute for Marine Resources Utilization, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), 2-15 Natsushima-cho, Yokosuka, Kanagawa 237-0061, Japan
²Frontier Research Center for Energy and Resources (FRCER), School of Engineering, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-8656, Japan
³Department of Planetology, Kobe University, 1-1 Rokkodai-cho, Nada-ku, Kobe, Hyogo 657-8501, Japan
⁴Ocean Resources Research Center for Next Generation, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba 275-0016, Japan

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¹Tack, P.,¹Bazi, B.,¹Vekemans, B.,²Okbinoglu, T.,³Van Maldeghem, F.,³Goderis, S.,²Schöder, S.,¹Vincze, L.
Journal of Synchotron Radiation 26, 2033-2039 Link to Article [DOI: 10.1107/S160057751901230X]
¹Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, 9000, Belgium
²PUMA Beamline, Synchrotron SOLEIL, Saint-Aubin BP48, Gif-sur-Yvette, F-91192, France
³Analytical-, Environmental- and Geo-chemistry, Vrije Universiteit Brussel, Pleinlaan 2, Brussels, 1000, Belgium

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¹S. D. Vance,¹M. Melwani Daswani
Philosophical Transactions of the Royal Society A 378, 2165 Link to Article [DOI:https://doi.org/10.1098/rsta.2018.0421]
¹Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8001, USA

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¹J.V. Clark,²B. Sutter,³A.C. McAdam,⁴E.B. Rampe,²P.D. Archer,⁴D.W. Ming,⁵R. Navarro‐Gonzalez,³P. Mahaffy,⁶T.J. Lapen
Journal of Geophysical Research, Planets (in Press) Link to Article [https://doi.org/10.1029/2019JE006173]
¹Geocontrols Systems – Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX
²Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX
³NASA Goddard Space Flight Center, Greenbelt, MD
⁴NASA Johnson Space Center, Houston, TX
⁵Universidad Nacional Autonoma de Mexico, Mexico City, Mexico
⁶University of Houston, Houston, TX
Published by arrangement with John Wiley & Sons

Evolved hydrogen chloride (HCl) detected by the Sample Analysis at Mars (SAM) instrument’s evolved gas analysis (EGA) mode on board the Mars Science Laboratory Curiosity rover has been attributed to oxychlorines (i.e., perchlorates and chlorates) or chlorides in Gale crater samples. Previous laboratory EGA studies of oxychlorines have been unable to reproduce the high‐temperature (>600 °C) HCl evolutions observed in most Gale crater samples. The objective of this work was to reproduce these high temperature HCl releases from laboratory mixtures of perchlorates and chlorides with phases that evolve water upon heating. Magnesium and sodium perchlorate and chloride were mixed with saponite, nontronite, and a basaltic glass and analyzed in a laboratory thermal evolved gas analyzer configured to operate similarly to the SAM instrument. Na perchlorate and chloride evolved HCl only when mixed with all three water‐producing phases. Mg perchlorate and chloride evolved a mid‐temperature HCl release (~450‐550 °C) and evolved an additional high‐temperature HCl release (~810‐820 °C) when mixed with saponite. This work demonstrated that chlorides, either originally present or from perchlorate decomposition, evolved high‐temperature HCl when reacting with water from water‐producing phases. The HCl release temperature was dependent on the mixture’s mineralogy and chemical composition. HCl releases detected by SAM were consistent with oxychlorines and/or chlorides in the presence of water‐producing phases. Additionally, this work provided constraints on the presence of oxychlorines or chlorides and their cation‐types, which has implications for past aqueous and diagenetic processes, the potential for past life, and detection of organics by EGA.

¹W. Crawford Elliott
American Mineralogist (2020) 105 (1): 1-2. Link to Article [https://doi.org/10.2138/am-2020-7312]
¹Department of Geosciences, Georgia State University, Atlanta, Georgia 30302-3965, U.S.A.

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¹Petrova, E.V.,¹Grokhovsky, V.I.
Pure and Applied Chemistry 91, 1857-1867 Link to Article [DOI: 10.1515/pac-2018-1119]
¹Ural Federal University, Institute of Physics and Technology, Ekaterinburg, Russian Federation

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¹Åke V. Rosén,^1,2Beda A. Hofmann,³Moritz von Sivers,^3,4Marc Schumann
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13427]
¹Institute of Geological Sciences, University of Bern, Baltzerstrasse 1+3, 3012 Bern, Switzerland
²Natural History Museum Bern, Bernastrasse 15, 3005 Bern, Switzerland
³Albert Einstein Center for Fundamental Physics, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
⁴Institute of Physics, University of Freiburg, Hermann‐Herder‐Strasse 3, 79104 Freiburg, Germany
Published by arrangement with John Wiley & Sons

Radionuclide activities were measured in the low‐background gamma‐ray spectrometry facility GeMSE in eight meteorite falls (Lost City, Tamdakht, Huaxi, Boumdeid, Xining, Kamargaon, Degtevo, and Ouidiyat Sbaa) and two finds (SaU 606 and Mürtschenstock) to evaluate the use of radionuclides for terrestrial age estimates. Results indicate that these meteorites were all derived from small‐ (r < 25 cm) to medium‐sized (r < 65 cm) meteoroids. Short‐lived ⁴⁸V (t_1/2 = 16.0 d) and ⁵¹Cr (t_1/2 = 27.7 d) were only detected in Oudiyat Sbaa (EH), while ⁷Be (t_1/2 = 53.1 d) was also detected in Degtevo (H) and Kamargaon (L), in agreement with reported fall dates. The ²²Na/²⁶Al activity ratio in Huaxi agrees with the previously reported short cosmic‐ray exposure age of this meteorite while ²²Na/²⁶Al in Kamargaon likely records a complex exposure history. Bayesian statistical analysis verifies the detection of very low activities of ⁴⁴Ti (t_1/2 = 60 a) in the relatively large H chondrites (>100 g) Degtevo, Huaxi, Tamdakht, Lost City, and SaU 606. Additionally, large samples from Oudiyat Sbaa (EH) and Kamargaon (L) gave positive detections. For H chondrite target compositions, detected ⁴⁴Ti(Fe+Ni)/²⁶Al averaged 0.055 ± 0.013. Activities of ²²Na and ⁵⁴Mn in SaU 606 show that this meteorite fell between July and September 2012, making SaU 606 the second recent fall from Oman identified using gamma‐ray spectrometry. The upper activity limit of ²²Na in the Mürtschenstock meteorite shows that it fell prior to 1999 and is not related to a bolide observation in 2015. Mürtschenstock shows ¹³⁷Cs ~10× higher than previously determined in Oman meteorites, likely due to Chernobyl fallout.

¹J. Nava,^2,3M. D. Suttle,¹R. Spiess,²L. Folco,³J. Najorka,⁴C. Carli,¹M. Massironi
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13429]
¹Department of Geosciences, University of Padova, Via G.Gradenigo 6, 35131 Padova, Italy
²Dipartimento di Scienze della Terra, Università di Pisa, 56126 Pisa, Italy
³Core Research Laboratories, Department of Earth Science, The Natural History Museum, Cromwell Rd, London, SW7 5BD UK
⁴IAPS‐INAF, Istituto Nazionale di Astrofisica e Planetologia Spaziali, Roma, Italy
Published by arrangement with John Wiley & Sons

TAM5.29 is an extraterrestrial dust grain, collected on the Transantarctic Mountains (TAM). Its mineralogy is dominated by an Fe‐rich matrix composed of platy fayalitic olivines and clasts of andradite surrounded by diopside‐jarosite mantles; chondrules are absent. TAM5.29 records a complex geological history with evidence of extensive thermal metamorphism in the presence of fluids at T < 300 °C. Alteration was terminated by an impact, resulting in shock melt veins and compaction‐orientated foliation of olivine. A second episode of alteration at lower temperatures (<100 °C) occurred postimpact and is either parent body or terrestrial in origin and resulted in the formation of iddingsite. The lack of chondrules is explained by random subsampling of the parent body, with TAM5.29 representing a matrix‐only fragment. On the basis of bulk chemical composition, mineralogy, and geological history TAM5.29 demonstrates affinities to the CV_ox group with a mineralogical assemblage in between the Allende‐like and Bali‐like subgroups (CV_oxA and TAM5.29 are rich in andradite, magnetite, and FeNiS, but CV_oxA lacks hydrated minerals, common in TAM5.29; conversely, CV_oxB are rich in hydrated phyllosilicates but contain almost pure fayalite, not found in TAM5.29). In addition, TAM5.29 has a slightly different metasomatic history, in between the oxidized and reduced CV metamorphic grades while also recording higher oxidizing conditions as compared to the known CV chondrites. This study represents the third CV‐like cosmic dust particle, containing a unique composition, mineralogy, and fabric, demonstrating variation in the thermal metamorphic history of the CV parent body(‐ies).