^1,2Xiaojia Zeng,^1,3Shijie Li,⁴Katherine H. Joy,^1,2,3 Xiongyao Li,^1,2,3Jianzhong Liu,^1,2,3Yang Li,^1,2Rui Li,⁵Shijie Wang
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13421]
¹Center for Lunar and Planetary Sciences, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081 China
²Key Laboratory of Space Manufacturing Technology, Chinese Academy of Sciences, Beijing, 100094 China
³CAS Center for Excellence in Comparative Planetology, Hefei, China
⁴Department of Earth and Environmental Sciences, University of Manchester, Manchester, M13 9PL UK
⁵State Key Laboratory of Environmental Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081 China
Published by arrangement with John Wiley & Sons

Lunar breccias preserve the records of geologic processes on the Moon. In this study, we report the occurrence, petrography, mineralogy, and geologic significance of the observed secondary olivine veinlets in lunar feldspathic breccia meteorite Northwest Africa (NWA) 11273. Bulk‐rock composition measurements show that this meteorite is geochemically similar to other lunar highland meteorites. In NWA 11273, five clasts are observed to host veinlets that are dominated by interconnecting olivine mineral grains. The host clasts are mainly composed of mafic minerals (i.e., pyroxene and olivine) and probably sourced from a basaltic lithology. The studied olivine veinlets (~5 to 30 μm in width) are distributed within the mafic mineral host, but do not extend into the adjacent plagioclase. Chemically, these olivine veinlets are Fe‐richer (Fo41.4–51.9), compared with other olivine grains (Fo54.3–83.1) in lithic clasts and matrix of NWA 11273. By analogy with the secondary olivine veinlets observed in meteorites from asteroid Vesta (howardite–eucrite–diogenite group samples) and lunar mare samples, our study suggests that the newly observed olivine veinlets in NWA 11273 are likely formed by secondary deposition from a lunar fluid, rather than by crystallization from a high‐temperature silicate melt. Such fluid could be sulfur‐ and phosphorous‐poor and likely had an endogenic origin on the Moon. The new occurrence of secondary olivine veinlets in breccia NWA 11273 reveals that the fluid mobility and deposition could be a previously underappreciated geological process on the Moon.

^1,2N.M.Curran,^1,3M.Nottingham,^3,4L.Alexander,^3,4I.A.Crawford,⁵E.Füri,¹K.H.Joy
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104823]
¹School of Earth and Environmental Sciences, University of Manchester, Oxford Road, Manchester, M13 9PL, UK
²NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD, 20771, USA
³Department of Earth and Planetary Science, Birkbeck College, University of London, London, UK
⁴The Centre for Planetary Sciences at UCL-Birkbeck, London, UK
⁵Centre de Recherches Pétrographiques et Géochimiques, CNRS-UL, 15 rue Notre Dame des Pauvres, BP20, 54501, Vandoeuvre-lès-Nancy Cedex, France

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¹Y.Langevin,²S.Merouane,²M.Hilchenbach,¹M.Vincendon,³K.Hornung,⁴C.Engrand,⁵ R.Schulz,²J.Kissel,⁶J.Ryno
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104815]
¹Institut d’Astrophysique Spatiale, CNRS/Univ. Paris Saclay, Orsay, France
²Max-Planck Institut für Sonnensystemforschung, Göttingen, Germany
³Universität der Bundeswehr, Neubiberg, Germany
⁴CSNSM, CNRS/Univ. Paris-Sud, Orsay, France
⁵European Space Agency Scientific Support Office, Noordwijk, the Netherlands
⁶Finnish Meteorological Institute, Helsinki, Finland

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¹Yoko Kebukawa,²Michael E.Zolensky,³Motoo Ito,⁴Nanako O.Ogawa, ⁴Yoshinori Takano,⁴ Naohiko Ohkouchi,⁵Aiko Nakato,⁶Hiroki Suga,⁷ Yasuo Takeichi,⁶Yoshio Takahashi,¹Kensei Kobayashi
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.12.012]
¹Faculty of Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya-ku, Yokohama 240-8501, Japan
²Astromaterials Research and Exploration Science, NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX 77058, USA
³Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology, B200 Monobe, Nankoku, Kochi 783-8502, Japan
⁴Biogeochemistry Program, Japan Agency for Marine-Earth Science and Technology, 2-15 Natsushima-Cho, Yokosuka 237-0061, Japan
⁵Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara 252-5210, Japan
⁶Department of Earth and Planetary Science, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
⁷Institute of Materials Structure Science, High-Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
Copyright Elsevier

Some xenolithic clasts in meteorites may have originated from unique primitive Solar System bodies. These clasts would provide novel insights into the early evolution of the Solar System. We conducted multiple analyses of organic matter (OM) in a CI-like xenolithic clast in the Zag (H5) meteorite including bulk elemental and isotopic analysis, FTIR, STXM/XANES, and NanoSIMS. The bulk C and N abundances in the Zag clast were +5.1 ± 0.4 wt.% and +0.26 ± 0.01 wt.%, respectively, which were the highest observed among various chondrite groups. The bulk δ¹³C value of the Zag clast was +23.0 ± 4.1 ‰ which was close to the value of the Tagish Lake meteorite; the δ¹⁵N value was +300 ± 3 ‰ which was close to the values of CR chondrites and Bells (a unique CM). The δD values of C-rich regions obtained by NanoSIMS were approximately +600 to +2000‰ which were close to the values of IOM from CI, CM and Tagish Lake. Some isotopic “hot spots” were observed with δD values up to ≈ +4000‰ and δ¹⁵N values up to ≈ +5500‰. The infrared transmission spectrum of the Zag clast was consistent with the abundant phyllosilicates and carbonates observed in the clast. The STXM showed abundant OM in various forms. C-XANES spectra from the OM were generally similar to CI/CM/CR chondrites. However, some variations existed in the molecular structures. OM in the Zag clast was partially associated with carbonates. The functional group, elemental and isotopic signatures of the OM in the Zag clast support the idea that the Zag clast is unique among known carbonaceous chondrite groups and originated from the outer Solar System such as aqueously-altered D/P type asteroids.

¹Wang, Y.-C.,^1,2Liu, Y.-X.,³Jiang, T.,¹Chen, K.-L.
Guang Pu Xue Yu Guang Pu Fen Xi/Spectroscopy and Spectral Analysis 39, 3154-3158 Link to Article [DOI: 10.3964/j.issn.1000-0593(2019)10-3154-05]
¹Institute of History of Metallurgy and Materials, University of Science and Technology Beijing, Beijing, 100083, China
²UCL Institute of Archaeology, London, WC1H0PY, United Kingdom
³Henan Provincial Institute of Archaeology and Cultural Relics, Zhengzhou, 450000, China

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¹Abdu, Y.A.
Journal of Physics: Conference Series 1258, 01230 Link to Article [DOI
https://doi.org/10.1088/1742-6596/1258/1/012030]
¹Department of Applied Physics and Astronomy, University of Sharjah, P.O. Box 27272, United Arab Emirates

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¹Sutton, S.R.,¹Lanzirotti, A.,¹Newville, M.,^2,3Dyar, M.D.,⁴Delaney, J.
Chemical Geology 531, 119305 Link to Article [DOI: 10.1016/j.chemgeo.2019.119305]
¹U. Chicago, IL, United States
²Planetary Science Institute, AZ, United States
³Mount Holyoke College, MA, United States
⁴Rutgers U., NJ, United States

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^1,2Bo-Magnus Elfers,^1,2,3Sprung Peter,^1,2 Messling Nils,^1,2Münker Carsten
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.12.008]
¹Institut für Geologie und Mineralogie, Universität zu Köln, Zülpicherstr. 49b, 50674 Cologne, Germany
²Steinmann-Institut, Rheinische Friedrich-Wilhelms-Universität Bonn, Poppelsdorfer Schloss, Meckenheimer Allee 169, 53115 Bonn, Germany
³Analytic Radioactive Materials, Hot Laboratory Division, Paul Scherrer Institute, 5232 Villigen, Switzerland
Copyright Elsevier

The stepwise acid digestion of primitive chondritic meteorites allows the identification of nucleosynthetic isotope anomalies that are otherwise hidden on the bulk rock scale. Here, we present for the first time combined isotope data for acid leachates, residues, and bulk rock aliquots of several primitive chondrites for the geo- and cosmochemically similar elements Zr and Hf. Our analyses reveal significant Zr and Hf isotope anomalies that (i) are complementary between acid leachates and residues and (ii) well-correlated with each other. The observed Zr and Hf anomalies strongly suggest variable contributions of common s-process carrier phases to the different leachates and residues. Ratios of r- (and p-process) Zr and Hf isotopes appear to be uniform in leachates and residues. In contrast to the well-correlated anomalies found in our leaching experiments, nucleosynthetic Zr and Hf isotope signatures seem to be decoupled on the bulk rock scale. This contrast may result from the heterogeneous distribution of neutron-rich Zr material devoid Hf, or alternatively be caused by the presence of anomalous CAI material which overprinted s-process deficits that were initially correlated.

In contrast to a previous study, we find no direct evidence for the presence of a third isotopically distinct nucleosynthetic Zr component.

^1,2Samira Frey et al. (>10)
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104816]
¹Space Research and Planetary Sciences, Physics Institute, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
²Laboratory for Astrophysics, Leiden Observatory, Leiden University, Niels Bohrweg 2, NL 2333, CA, Leiden, the Netherlands

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¹P.R.Kumaresan,¹J.Saravanavel,¹K.Palanivel
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104817]
¹Departmentof Remote Sensing, Bharathidasan University -Khajamalai Campus, Tiruchirappalli, 620 023, Tamil Nadu, India

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