¹Gargulák, M.,²Ozdín, D.,³Povinec, P.P.,^4,5Strekopytov, S.,^6,7Timothy Jull, A.J.,³Sýkora, I.,⁹Porubčan, V.,¹⁰Farsang, S.
Geologica Carpathica 71, 221-232 Link to Article [DOI: 10.31577/GeolCarp.71.3.2]
¹State Geological Institute of Dionýz Štúr, Mlynská dolina 1, Bratislava 11, 817 04, Slovakia
²Comenius University, Faculty of Natural Sciences, Department of Mineralogy and Petrology, Ilkovičova 6, Bratislava 4, 842 15, Slovakia
³Comenius University, Faculty of Mathematics, Physics and Informatics, Department of Nuclear Physics and Biophysics, Mlynská dolina, Bratislava, 842 48, Slovakia
⁴Natural History Museum, Imaging and Analysis Centre, Cromwell Road, London, SW7 5BD, United Kingdom
⁵National Measurement Laboratory, LGC, Queens Road, Teddington, TW11 0LY, United Kingdom
⁶University of Arizona, Department of Geosciences, Tucson, AZ 85721, United States
⁷Isotope Climatology and Environmental Research Centre, Hungarian Academy of Sciences, Institute for Nuclear Research, Debrecen, 4026, Hungary
⁸Astronomical Institute, Slovak Academy of Sciences, Dúbravská cesta 9, Bratislava, 845 04, Slovakia
⁹University of Cambridge, Department of Earth Sciences, Downing Street, Cambridge, CB2 3EQ, United Kingdom

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^1,2Fernini, I. et al. (>10)
Journal of Instrumentation 15, T06007 Link to Article [DOI: 10.1088/1748-0221/15/06/T06007]
¹Sharjah Academy for Astronomy, Space Sciences, and Technology (SAASST), University of Sharjah, Sharjah, United Arab Emirates
²Applied Physics and Astronomy Department, University of Sharjah, Sharjah, United Arab Emirates

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^1,2Wang, X.-F.,²Wu, B.,¹Liu, J.-B.,²Kong, D.-F.,¹Li, S.-T.,¹Wang, F.
Gongcheng Lixue/Engineering Mechanics 37, 237-241 Link to Article [DOI: 10.6052/j.issn.1000-4750.2019.04.S044]
¹Department of Civil Engineering, Tsinghua University, Beijing, 100084, China
²Research Institute for National Defense Engineering of Academy of Military Science PLA China, Luoyang, Henan 471023, China

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¹Mahajan, R.R.
Earth, Moon and Planets 124, 3-13 Link to Article [DOI: 10.1007/s11038-020-09532-w]
¹Physical Research Laboratory, Ahmedabad, 380009, India

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¹Maksimova, A.A.,¹Petrova, E.V.,¹Chukin, A.V.,²Karabanalov, M.S.,³Nogueira, B.A.,³Fausto, R.,⁴Yesiltas, M.,⁵Felner, I.,¹Oshtrakh, M.I.
Spectrochimica Acta – Part A: Molecular and Biomolecular Spectroscopy 242, 118723 Link to Article [DOI: 10.1016/j.saa.2020.118723]
¹Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation
²Institute of Material Science and Metallurgy, Ural Federal University, Ekaterinburg, 620002, Russian Federation
³CQC, Department of Chemistry, University of Coimbra, Coimbra, 3004-535, Portugal
⁴Faculty of Aeronautics and Space Sciences, Kirklareli University, Kirklareli, Turkey
⁵Racah Institute of Physics, The Hebrew University, Jerusalem, Israel

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¹Peng Ni,²Nancy L. Chabot,²Caillin J. Ryan,¹Anat Shahar
Nature Geoscience (in Press) Link to Article [DOI
https://doi.org/10.1038/s41561-020-0617-y]
¹Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
²Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA

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^1,2Morgan A. Cox et al. (>10)
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13541]
¹Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, Western Australia, 6102 Australia
²Lunar and Planetary Institute (LPI)—USRA, 3600 Bay Area Boulevard, Houston, Texas, 77058 USA
Published by arrangement with John Wiley & Sons

The mineral apatite, Ca5(PO4)3(F,Cl,OH), is a ubiquitous accessory mineral, with its volatile content and isotopic compositions used to interpret the evolution of H2O on planetary bodies. During hypervelocity impact, extreme pressures shock target rocks resulting in deformation of minerals; however, relatively few microstructural studies of apatite have been undertaken. Given its widespread distribution in the solar system, it is important to understand how apatite responds to progressive shock metamorphism. Here, we present detailed microstructural analyses of shock deformation in ~560 apatite grains throughout ~550 m of shocked granitoid rock from the peak ring of the Chicxulub impact structure, Mexico. A combination of high‐resolution backscattered electron (BSE) imaging, electron backscatter diffraction mapping, transmission Kikuchi diffraction mapping, and transmission electron microscopy is used to characterize deformation within apatite grains. Systematic, crystallographically controlled deformation bands are present within apatite, consistent with tilt boundaries that contain the (axis) and result from slip in <> (direction) on (plane) during shock deformation. Deformation bands contain complex subgrain domains, isolated dislocations, and low‐angle boundaries of ~1° to 2°. Planar fractures within apatite form conjugate sets that are oriented within either {, {, {, or . Complementary electron microprobe analyses (EPMA) of a subset of recrystallized and partially recrystallized apatite grains show that there is an apparent change in MgO content in shock‐recrystallized apatite compositions. This study shows that the response of apatite to shock deformation can be highly variable, and that application of a combined microstructural and chemical analysis workflow can reveal complex deformation histories in apatite grains, some of which result in changes to crystal structure and composition, which are important for understanding the genesis of apatite in both terrestrial and extraterrestrial environments.

¹Edouard Kaminski,¹Angela Limare,¹ Balthasar Kenda,¹Marc Chaussidon
Earth and Planetary Science 548, 116469 Link to Article [https://doi.org/10.1016/j.epsl.2020.116469]
¹Université de Paris, Institut de Physique du Globe de Paris, CNRS, 1 rue Jussieu, F-75005 Paris, France
Copyright Elsevier

The timing of formation of 100-300 km size planetesimals in the protoplanetary disk remains largely unconstrained. Recent models show that gravitational collapse of boulders in overdense regions of a dusty accretion disk can overcome the meter-sized barrier and lead to rapid formation of planetesimals with size of several km that further grow by pebble accretion. Hf/W ages indicate that the first large planetesimals to form could be the parent bodies of magmatic iron meteorites. These ages have been so far used to constrain timing of accretion considering (i) instantaneous accretion, and (ii) purely conductive heat transfer in the planetesimal. To relax these hypotheses we model the thermal evolution of a planetesimal in course of accretion and we take into account the possibility of convection onset. Our model is further based on considering the possibility of a common thermal evolution for all the parent bodies of iron meteorites. Within that framework we show that the planetesimals could have grown following a universal accretion law starting at the very beginning of the history of the disk by a nearly instantaneous formation of 60 ± 30 km size nuclei, followed by a growth via pebble accretion at a much slower pace to reach final sizes of 150–300 km in about 3 Myr. In this universal scenario, complete melting and total differentiation are not bound to happen in the parent body due to the continuous accretion of cold pebbles. The model, though calibrated here on iron meteorites, is general and can in principle be applied to other types of planetesimals such as for instance the parent bodies of CV chondrites.

¹Dennis Harries,²Addi Bischoff
Earth and Planetary Science Letters 548, 116506 Link to Article [https://doi.org/10.1016/j.epsl.2020.116506]
¹Institute für Geowissenschaften, Friedrich-Schiller-Universität Jena, Carl-Zeiss-Promenade 10, 07745 Jena, Germany
²Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Str. 10, 48149, Münster, Germany
Copyright Elsevier

Two samples of a unique achondritic lithology of the Almahata Sitta meteorite (MS-MU-019 and MS-MU-036) contain three coexisting pyroxene species: orthoenstatite, clinoenstatite and augite. The silicate assemblage appears to be the restite after extraction of melts of broadly basaltic and metal-sulfide composition from an enstatite chondrite protolith. Transmission electron microscopy (TEM) provides evidence that clinoenstatite within the lithology formed from earlier protoenstatite. The absence of pigeonite despite the successful nucleation of augite and the persistence of orthoenstatite during cooling suggests that the sub-solidus formation of the three coexisting pyroxenes occurred at a pressure of about 0.1 GPa. Rapid cooling at >1 K/h below 1260°C is documented by the cessation of augite equilibration, preservation of the 3-pyroxene assemblage and a low volume fraction of nanoscale orthoenstatite lamellae formed during the transformation of protoenstatite to clinoenstatite. The pressure implies a diameter of roughly 500 km of the differentiated parent body, putting petrological constraints on the size of planetesimals that may have contributed to the accretion of the terrestrial planets including Earth. The high cooling rate indicates a catastrophic disruption of this large planetesimal early in its history. The lithology studied here underlines that planetesimals which existed in the inner Solar System were more diverse than previously thought, and included potentially large differentiated bodies with very FeO-poor, enstatite-dominated mantles. Remains of these bodies are poorly represented in meteorite collections, which points to efficient accretion in the inner Solar System or to removal and little re-distribution of material into the present-day asteroid belt.

¹James M. D. Day
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13544]
¹Scripps Institution of Oceanography, University of California San Diego, La Jolla, California, 92093 USA
Published by arrangement with John Wiley & Sons

Anhedral metal grains of >micrometer size occur in many lunar rock types, including mare basalts, magnesian suite rocks (MGS), ferroan anorthosites (FAN), and impact melt rocks and breccias. Some metal grains are inherited from, or modified by, impactors striking the Moon into crustal materials. These grains have high Ni/Co resulting from the addition of chondritic or iron impactors. Metal grains in mare basalts, FAN, and MGS have Ni/Co ranging from >20 to <1, being generally distinct from impactor compositions. Nickel and Co behave as compatible elements in lunar melts, with parental melts having between ~40–50 ppm Co, ~40–60 ppm Ni, and Ni/Co ~1. These compositions suggest a bulk silicate Moon (BSM) with Ni some three times lower than in bulk silicate Earth. Modeling of Ni and Co during fractional crystallization of mafic mare basalt parental melts originating from a BSM source predicts high Ni/Co metals form during early olivine fractionation. The combined effects of pyroxene ± plagioclase crystallization and increasing but variable compatibility of Ni and Co during basaltic melt evolution can explain the generation of low Ni/Co metals in more differentiated mare basalts. High‐Ti mare basalts have metal with low Ni/Co, but the crystallization of ilmenite and armalcoite restricts the range of Ni and Co in metal. Collectively, these results are consistent with metal grains in mare basalts forming solely through endogenous processes. Measurement of metal grains represents a rapid way for determining endogenous (e.g., lunar interior melts) versus exogenous (e.g., impact contamination) processes acting on lunar samples. In turn, the presence of low Ni/Co metal grains in mare basalts supports their origin as uncontaminated partial melts originating from lunar mantle sources that may have experienced loss of Ni to a small lunar core.