^1,2,3Poole, Graeme M.,¹Stumpf, Roland,¹Rehkämper, Mark
Journal of Analytical Atomic Spectrometry 37, 783-794 Open Access Link to Article [DOI 10.1039/d1ja00468a]
¹Department of Earth Science and Engineering, Imperial College London, London, SW7 2AZ, United Kingdom
²School of Earth Sciences, University of Bristol, Bristol, BS8 1RJ, United Kingdom
³Imaging and Analysis Centre, Natural History Museum, London, SW7 5BD, United Kingdom

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Tian, Shengyu,¹Moynier, Frederic,¹Inglis, Edward C.,²Jensen, Ninna K.,²Deng, Zhengbin,²Schiller, Martin,^1,2Bizzarro, Martin
Journal of Analytical Atomic Spectrometry 37, 656 – 662 Link to Article [DOI 10.1039/d1ja00418b]
¹Université de Paris, Institut de Physique Du Globe de Paris, CNRS, Paris cedex 05, France
²Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Greber, Nicolas D.,³Van Zuilenc, Kirsten
Chimia 76, 18-25 Open Access Link to Article [DOI 10.2533/chimia.2022.18]
¹Natural History Museum of Geneva, Route de Malagnou 1, Geneva, CH-1208, Switzerland
²Institute of Geological Sciences, University of Bern, Baltzerstrasse 1+3, Bern, CH-3012, Switzerland
³Vrije Universiteit, De Boelelaan 1085, Amsterdam, 1081 HV, Netherlands

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Wieler, Rainer
Chimia 76, 9-17 Open Access Link to Article [DOI 10.2533/chimia.2022.9]
¹ETH Zürich, Department of Earth Sciences, Clausiusstrasse 25, Zurich, CH-8092, Switzerland

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Damanveer S.Grewal,¹Tao Sun,^1,3Sanath Aithala,¹Taylor Hough,¹Rajdeep Dasgupta,^1,4Laurence Y.Yeung,⁵Edwin Schauble
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2022.10.025]
¹Department of Earth, Environmental and Planetary Sciences, Rice University, 6100 Main Street, MS 126, Houston, TX 77005, USA
²Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA
³Department of Earth and Environmental Sciences, University of Minnesota, Minneapolis, MN 55455, USA
⁴Department of Chemistry, Rice University, 6100 Main Street, MS 126, Houston, TX 77005, USA
⁵Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, USA
Copyright Elsevier

15N/14N ratios of meteorites are a powerful tool for tracing the journey of life-essential volatiles like nitrogen (N), carbon and water from nebular solids to the present-day rocky planets, including Earth. The utility of 15N/14N ratios of samples originating from differentiated protoplanets (e.g., iron meteorites) and planets (e.g., Earth’s mantle) for tracing this journey could be affected by the fractionation of N isotopes during core-mantle differentiation, which would overprint their primitive compositions. The extent of N isotopic fractionation during core-mantle differentiation and its effect on the 15N/14N ratios of resulting metallic and silicate reservoirs is, however, poorly understood. Using high pressure-temperature experiments, here we show that N isotopic fractionation between metallic and silicate melts (Δ15Nalloy–silicate = δ15Nalloy – δ15Nsilicate = –3.3‰ to –1.0‰) is limited across a wide range of oxygen fugacity and is much smaller than previous estimates. Also, we present ab initio calculations based on the relevant N speciation in metallic and silicate melts confirming both the magnitude and direction of N isotopic fractionation predicted by our experimental results. Limited N isotopic fractionation during core-mantle differentiation suggests that the core and mantle relicts largely preserve the N isotopic compositions of their bulk bodies. Based on the δ15N values of non-carbonaceous iron meteorites (as low as –95‰), we predict that the extent of variations in the N isotopic compositions of inner solar system protoplanets was larger than that recorded by enstatite chondrites (δ15N = –29‰ to –6‰). As most of the Earth grew primarily via the accretion of similar inner solar system protoplanets, a relatively high δ15N value of present-day Earth’s primitive mantle (–5‰) cannot be explained by the accretion of enstatite chondrite-like materials alone and necessitates a significant contribution of 15N-rich materials to the Earth’s interior.

¹Ohara, Satoshi,²Naka, Takashi,³Hashishin, Takeshi
Science Advances 8, eabj2487 Open Access Link to Article [DOI 10.1126/sciadv.abj2487]
¹Joining and Welding Research Institute, Osaka University, 11-1 Mihogaoka, Osaka, Ibaraki, 567-0047, Japan
²National Institute for Materials Science, 1-2-1 Sengen, Ibaraki, Tsukuba, 305-0047, Japan
³Division of Materials Science and Chemistry, Faculty of Advanced Science and Technology, Division of Surface and Grain Boundary, Institute of Industrial Nanomaterials, Kumamoto University, 2-39-1 Kurokami, Chuo-ku, Kumamoto, Kumamoto, 860-8555, Japan

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Elkins-Tanton, Linda T. et al. (>10)
Space Science Reviews 218, 17 Open Access Link to Article [DOI 10.1007/s11214-022-00880-9]
¹School of Earth and Space Exploration, Arizona State University, Tempe, 86387-2001, AZ, United States

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Miles Lindner,^1,2Dominik C. Hezel,^1,2Axel Gerdes,^1,2Horst R. Marschall,^1,3Frank E. Brenker
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.13917]
¹Institut für Geowissenschaften, Goethe-Universität Frankfurt, Altenhöferallee 1, 60438 Frankfurt am Main, Germany
²Frankfurt Isotope and Element Research Center (FIERCE), Goethe Universität, 60438 Frankfurt am Main, Germany
³Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, Hawaii, 96822 USA
Published by arrangement with John Wiley & Sons

Enriched shergottites contain interstitial Si-rich mesostasis; however, it is unclear whether such mesostasis is formed by impact or magmatic processes. We use laser ablation multicollector inductively coupled plasma mass spectrometry U–Pb measurements of minerals within the interstitial Si-rich mesostasis and of merrillite within the coarse-grained groundmass of Martian-enriched gabbroic shergottite Northwest Africa (NWA) 6963. The date derived of tranquillityite, Cl-apatite, baddeleyite, and feldspar from the Si-rich mesostasis is 172.4 ± 6.1 Ma, and the derived merrillite date is 178.3 ± 10.6 Ma. We conclude, based on textural observation, that merrillite is a late magmatic phase in NWA 6963, that it was not produced by shock, and that its U–Pb-system was not reset by shock. The indistinguishable dates of the gabbroic merrillite and the minerals within the Si-rich mesostasis in NWA 6963 indicate that the Si-rich mesostasis represents a late-stage differentiated melt produced in the final phase of the magmatic history of the gabbroic rock and not a shock melt. This can likely be transferred to similar Si-rich mesostases in other enriched shergottites and opens the possibility for investigations of Si-rich mesostasis in enriched shergottites to access their magmatic evolution. Our results also provide a crystallization age of 174 ± 6 Ma (weighted average) for NWA 6963.

¹Deze Liu,¹Frédéric Moynier,^1,2Julien Siebert,^1,3Paolo A.Sossi,¹Yan Hu,¹Edith Kubik
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2022.09.043]
¹Université Paris Cité, Institut de Physique du Globe de Paris, 1 Rue Jussieu, 75005 Paris, France
²Institut Universitaire de France, Paris, France
³Institute of Geochemistry and Petrology, ETH Zürich, Sonneggstrasse 5, CH-8092 Zürich, Switzerland
Copyright Elsevier

In comparison with the Sun and CI chondrites, moderately volatile elements (MVEs) are depleted in terrestrial planets and other small, rocky differentiated bodies in the inner solar system. The abundances of most MVEs in the bulk silicate Earth (BSE) fall on a trend that defines a near log-linear decrease with their 50% nebular condensation temperature (). This temperature scale has traditionally been used to infer elemental volatility during planetary formation and accretion, however, indium (In) deviates from this correlation. Despite being a siderophile element that could have been depleted by core formation, In is overabundant for its calculated in the BSE, as well as in the silicate portions of other small bodies (e.g., Moon and Vesta). This overabundance of In indicates that , calculated under nebular conditions, may not be applicable to planetary evaporation that occurs at much higher oxygen fugacity (fO2) and pressure than nominal nebular conditions. Here, we conduct a series of evaporation experiments for basaltic melts to quantify the volatility of In under conditions relevant to planetary evaporation. Our results show that, when using the evaporation temperature , refers to the temperature at which 1% of element i has evaporated from liquid to gas phase under equilibrium) as the volatility scale, the abundances of volatile elements, including In, of the Moon and Vesta display a progressive depletion with increasing volatility (decreasing ). This smooth depletion pattern contrasts with the overabundance of In shown on the scale, suggesting that volatile depletion on small bodies occurred under non-nebular environment instead of during nebular condensation. On the other hand, the volatile element composition of the BSE (including In) could be explained by integrating i) early accreted precursor materials of the proto-Earth that underwent volatile loss under conditions more oxidizing than those of the solar nebula with ii) late added volatile-rich materials.

¹Kvasnytsya, Victor M.,²Wirth, Richard
Mineralogy and Petrology 116, 169 – 187 Link to Article [DOI
10.1007/s00710-022-00778-y]
¹Semenenko Institute of Geochemistry, Mineralogy and Ore Formation, National Academy of Sciences of Ukraine, pr. Akademika Palladina 34, Kyiv, 03142, Ukraine
²Helmholtz Center Potsdam and German Research Center for Geosciences, Section 3.5 Interface Geochemistry, Telegrafenberg, Potsdam, 14473, Germany

We currently do not have a copyright agreement with this publisher and cannot display the abstract here