¹Qi, Xiaobin,^1,2Ling, Zongcheng,¹Liu, Ping,¹Chen, Jian,¹Cao, Haijun,¹Liu, Changqing,¹Wang, Xiaoyu,¹Liu, Yiheng
Eartzh and Space Science 10, e2023EA002825 Open Access Link to Article [DOI 10.1029/2023EA002825]
¹Shandong Key Laboratory of Optical Astronomy and Solar—Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, Weihai, China
²CAS Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei, China

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^1,2,3Gerrit ³ L.H. Tissot,^2,4Thorsten Kleine,³Ren T. Marquez
Geochemistry (Chemie der Erde) (in Press) Link to Article [https://doi.org/10.1016/j.chemer.2023.126007]
¹Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
²Institut für Planetologie, University of Münster, 48149 Münster, Germany
³The Isotoparium, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
⁴Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
Copyright Elsevier

Mass-independent (nucleosynthetic) Mo isotope anomalies are uniquely useful for constraining genetic relationships among meteoritic and planetary materials and, by extension, the origin and nature of Earth’s late-stage building blocks. The meaningful interpretation of such data, however, critically depends on the accurate correction of any natural and analytical mass-dependent isotope fractionation, which is commonly assumed to follow the ‘exponential law’. Here, using new high-precision Mo isotope data for a diverse set of terrestrial samples, we show that mass-dependent Mo isotope fractionation in nature typically does not adhere to this law, but is instead dominated by equilibrium and Rayleigh processes. We demonstrate that even moderate degrees of such non-exponential fractionation (i.e., mass-dependent isotope fractionation deviating from the exponential law) can result in significant spurious mass-independent Mo isotope anomalies that, when misinterpreted as nucleosynthetic anomalies, can lead to erroneous conclusions, particularly with respect to Earth’s accretion history. Consequently, assessing the magnitude and origin of mass-dependent fractionation will be essential for future efforts to precisely determine the mass-independent Mo isotope composition of bulk silicate Earth and to identify potential nucleosynthetic isotope anomalies in terrestrial rocks.

^1,2Tang, Xuhai,¹Xu, Jingjing,¹Zhang, Yiheng,³Zhao, Haifeng,⁴Paluszny, Adriana,³Wan, Xue,¹Wang, Zhengzhi
Engineering Geology 321, 107154 Link to Article [DOI 10.1016/j.enggeo.2023.107154]
¹School of Civil Engineering, Wuhan University, Hubei, Wuhan, 430072, China
²Wuhan University Shenzhen Research Institute, Shenzhen, 518057, China
³Technology and Engineering Center for Space Utilization, Chinese Academy of Sciences, Beijing, 100094, China
⁴Department of Earth Science and Engineering, Imperial College, London, United Kingdom#

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^1,2Peters, Sophia,^1,2Semenov, Dmitry A.,³Hochleitner, Rupert,^1,2Trapp, Oliver
Scientific Reports (in Press) Open Access Link to Article [DOI 10.1038/s41598-023-33741-8]
¹Department of Chemistry, Ludwig-Maximilians-Universität München, Butenandtstr. 5-13, Munich, 81377, Germany
²Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany
³Mineralogische Staatssammlung München, Theresienstr. 41, Munich, 80333, Germany

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¹Yumoto, Koki, ¹Cho, Yuichiro, ^2,3Kameda, Shingo, ¹Kasahara, Satoshi, ^1,4,5Sugita, Seiji
Spectrochimica Acta – Part B Atomic Spectroscopy 205, 106696 Link to Article [DOI
10.1016/j.sab.2023.106696]
¹Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, 113-0033, Japan
²Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo, 171-8501, Japan
³Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Kanagawa, Sagamihara, 252-5210, Japan
⁴Research Center of Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, 113-0033, Japan
⁵Planetary Exploration Research Center, Chiba Institute of Technology, Narashino, 275-0016, Japan

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^1,2V. Fortier,²V. Debaille,^1,3V. Dehant,⁴B. Bultel
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2023.105749]
¹Earth and Life Institute, Université Catholique de Louvain-la-Neuve, Louvain-la-Neuve, Belgium
²Laboratoire G-Time, Université libre de Bruxelles, Bruxelles, Belgium
³Royal Observatory of Belgium, Bruxelles, Belgium
⁴Geosciences Paris Saclay, Université Paris-Saclay, Paris, France

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¹R. J. Curtis,¹H. C. Bates,¹T. J. Warren,¹K. A. Shirley,¹E. C. Brown,¹A. J. King,¹N. E. Bowles
Meteoritics & Planetary Scince (in Press) Link to Article [https://doi.org/10.1111/maps.14055]
¹Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK
²Earth Sciences, Natural History Museum, London, UK
Published by arrangement with John Wiley & Sons

A laboratory study was performed using the Visible Oxford Space Environment Goniometer in which the broadband (350–1250 nm) bidirectional reflectance distribution function (BRDF) of the Winchcombe meteorite was measured, across a range of viewing angles—reflectance: 0°–70°, in steps of 5°; incidence: 15°, 30°, 45°, and 60°; and azimuthal: 0°, 90°, and 180°. The BRDF dataset was fitted using the Hapke BRDF model to (1) provide a method of comparison to other meteorites and asteroids, and (2) to produce Hapke parameter values that can be used to extrapolate the BRDF to all angles. The study deduced the following Hapke parameters for Winchcombe: w = 0.152 ± 0.030, b = 0.633 ± 0.064, and h_S = 0.016 ± 0.008, demonstrating that it has a similar w value to Tagish Lake (0.157 ± 0.020) and a similar b value to Orgueil (0.671 ± 0.090). Importantly, the surface profile of the sample was characterized using an Alicona 3D® instrument, allowing two of the free parameters within the Hapke model φ and �¯, which represent porosity and surface roughness, respectively, to be constrained as φ = 0.649 ± 0.023 and �¯ = 16.113° (at 500 μm size scale). This work serves as part of the characterization process for Winchcombe and provides a reference photometry dataset for current and future asteroid missions.

¹Guy Libourel,²Pierre Beck,³Akiko M. Nakamura,⁴Pierre Vernazza,⁵Clement Ganino,¹Patrick Michel
The Planetary Science Journal 4, 123 Open Access Link to Article [DOI 10.3847/PSJ/ace114]
¹Université Côte d’Azur, Lagrange, Observatoire de la Côte d’Azur, CNRS, Nice, France
²UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, Grenoble, France
³Graduate School of Science, Kobe University, Japan
⁴Université Aix-Marseille, CNRS, Laboratoire d’Astrophysique de Marseille, Marseille, France
⁵Université Côte d’Azur, Géoazur, Observatoire de la Côte d’Azur, CNRS, Valbonne, France

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¹Aimee Smith,¹Rhian H. Jones
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.14051]
¹Department of Earth and Environmental Sciences, The University of Manchester, Manchester, UK
Published by arrangement with John Wiley & Sons

In the CR (Renazzo-like) chondrite group, many chondrules have successive igneous rim (IR) layers, with an outer layer that contains a silica mineral and/or silica-rich glass (silica-rich igneous rims, SIRs). Models for SIR formation include (1) accretion of Si-rich dust onto solid chondrule surfaces, followed by heating and cooling and (2) condensation of SiO(gas) onto the surface of partially molten chondrules. We evaluate these models, based on a petrographic study of five Antarctic CR chondrites that have undergone minimal secondary alteration. We obtained electron microprobe analyses of minerals and glass with quantitative wavelength-dispersive spectroscopy mapping, and identified silica polymorphs with Raman spectroscopy. Common SIRs contain silica, low-Ca pyroxene, Ca-rich pyroxene, Fe,Ni metal, ± glass ± plagioclase ± rare olivine. We also describe near-monomineralic SIRs where a narrow zone of cristobalite occurs at the outer edge of the chondrule. All crystalline silica is cristobalite, except for one SIR that consists of tridymite. Some rims contain silica-rich glass (>80 wt% SiO2) but no silica mineral. Features such as sharp interfaces and compositional boundaries between chondrules and SIRs indicate that SIRs were formed from solid precursors. Consideration of the stability fields of silica polymorphs and computed liquidus temperatures indicates that SIRs were heated to >1500°C for limited time periods, followed by rapid cooling, similar to conditions for chondrule formation. We infer that in the CR chondrule formation region, the same heating mechanism was repeated multiple times while the chemical composition of the nebular gas evolved to highly fractionated silica-rich compositions.

¹Isaac J. Onyett,¹Martin Schiller,¹Georgy V. Makhatadze,¹Zhengbin Deng,^1,2Anders Johansen,^1,3Martin Bizzarro
Nature 619, 539-544 Open Access Link to Article [DOI https://doi.org/10.1038/s41586-023-06135-z]
¹Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
²Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Lund, Sweden
³Institut de Physique du Globe de Paris, Université de Paris Cité, Paris, France

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