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1. A reassessment of the iron isotope composition of the Moon and its implications for the accretion and differentiation of terrestrial planets

Author

Tomáš Magna, Franck Poitrasson, Clive R. Neal, Thomas Zambardi, Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Basalt, Olivine, 010504 meteorology & atmospheric sciences, Stable isotope ratio, Lunar mare, Geochemistry, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Mantle (geology), Isotope fractionation, Planetary science, 13. Climate action, Geochemistry and Petrology, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, engineering, Terrestrial planet, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The Fe isotope composition of planetary bodies may provide constraints on their accretion modes and/or differentiation processes, but to do so, the Fe isotope systematics of key planetary reservoirs needs to be determined. To investigate this for the Moon, we measured the Fe isotope compositions for a suite of 33 bulk lunar mare basalts and highland rocks. Combined with published data, a compendium of 73 different lunar bulk rocks reveals a statistically significant Fe isotope difference between low-Ti and high-Ti mare basalts, yielding average δ57Fe = 0.127 ± 0.012‰ (2SE; n = 27) and δ57Fe = 0.274 ± 0.020‰ (2 SE; n = 25), respectively, relative to the IRMM-14 isotopic reference material. As lunar basalts are thought to reflect the Fe isotope composition of their respective mantle sources, the estimated relative proportion of the low-Ti and high-Ti source mantle suggests that the lunar upper mantle δ57Fe value should be close to 0.142 ± 0.026‰. Whilst the composition of highland rocks (ferroan anorthosites and Mg-suite rocks) should provide a more global view of the Moon, the calculation of the mean δ57Fe value of 15 available highland rock analyses yields δ57Fe = 0.078 ± 0.124‰. Such a value is not defined precisely enough to be of critical use for comparative planetology. Ferroan anorthosites and Mg-suite rocks also give unresolvable means. It appears that Fe isotope heterogeneity among the lunar highland rocks is caused by non-representatively too small sample aliquots of coarse-grained rocks. It can also be the result of mixed lithologies for some. When the (kinetic) effect of olivine tending towards low δ57Fe and feldspar with predominantly high δ57Fe is cancelled, a more precise δ57Fe value of 0.094 ± 0.035‰ is calculated. It is indistinguishable from the mean δ57Fe of impact melts and is also similar to the upper lunar mantle estimate obtained from mare basalts. Collectively, this newly determined Fe isotope composition of the bulk Moon is indistinguishable from that of the Earth, and heavier than those reported for other planetary bodies. This planetary isotope relationship is only observed for silicon given the currently available mass-dependent stable isotope database. Because both iron and silicon reside in the Earth’s metallic core in significant quantities, this may point to the involvement of metallic cores of the Earth and Moon in the interplanetary Fe and Si isotope fractionation. Rather than via high-pressure metal–silicate fractionation at the core–mantle boundary, this would more likely be achieved by partial vaporization of the liquid outer metallic core in the aftermath of a Moon-forming giant impact.

Published
2019
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2. Martian magmatism from plume metasomatized mantle

Author

Clive R. Neal, Frédéric Moynier, Arya Udry, James M.D. Day, Kimberly T. Tait, Yang Liu, Scripps Institution of Oceanography (SIO), University of California [San Diego] (UC San Diego), University of California-University of California, Royal Ontario Museum, University of Nevada [Las Vegas] (WGU Nevada), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and University of Notre Dame [Indiana] (UND)

Subjects
010504 meteorology & atmospheric sciences, SM-ND, Science, Geochemistry, General Physics and Astronomy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ISOTOPIC SYSTEMATICS, 010502 geochemistry & geophysics, DEPLETED MANTLE, 01 natural sciences, Article, General Biochemistry, Genetics and Molecular Biology, Mantle (geology), Mantle plume, DIFFERENTIATION HISTORY, Lithosphere, Nakhlite, MAUNA-KEA VOLCANO, Composition of Mars, lcsh:Science, REJUVENATED VOLCANISM, 0105 earth and related environmental sciences, Martian, Multidisciplinary, RB-SR, Partial melting, MARS, General Chemistry, Meteorite, 13. Climate action, HAWAIIAN HOT-SPOT, lcsh:Q, MIDOCEAN RIDGE BASALT, Geology
Abstract

Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here we report a coherent geochemical dataset for shergottites, nakhlites and chassignites revealing fundamental differences in sources. Shergottites have lower Nb/Y at a given Zr/Y than nakhlites or chassignites, a relationship nearly identical to terrestrial Hawaiian main shield and rejuvenated volcanism. Nakhlite and chassignite compositions are consistent with melting of hydrated and metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep mantle sources. Generation of martian magmas can be explained by temporally distinct melting episodes within and below dynamically supported and variably metasomatized lithosphere, by long-lived, static mantle plumes., A unified model for the formation of martian rock types is required to understand Mars’s formation and evolution. Here the authors show that nakhlite and chassignite meteorites originate from melting of metasomatized depleted mantle lithosphere, whereas shergottite melts originate from deep plume sources.

Published
2018
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3. Early degassing of lunar urKREEP by crust-breaching impact(s)

Author

Francis M. McCubbin, Ian A. Franchi, Romain Tartèse, Jessica Barnes, Clive R. Neal, Mahesh Anand, Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Earth Sciences department [London], The Natural History Museum [London] (NHM), NASA Johnson Space Center (JSC), NASA, Department of Civil and Environmental Engineering and Earth Science [Notre Dame] (CEEES), University of Notre Dame [Indiana] (UND), and Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Geochemistry, KREEP, Mineralogy, Context (language use), 010502 geochemistry & geophysics, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), NanoSIMS, Moon, 0105 earth and related environmental sciences, Isotope, Rare-earth element, Isotopes of chlorine, Crust, magma ocean, Geophysics, volatiles, Lunar magma ocean, 13. Climate action, Space and Planetary Science, apatite, chlorine, Earth (classical element), Geology
Abstract

Current models for the Moon’s formation have yet to fully account for the thermal evolution of the Moon in the presence of H2O and other volatiles. Of particular importance is chlorine, since most lunar samples are characterised by unique heavy δ37Cl values, significantly deviating from those of other planetary materials, including Earth, for which δ37Cl values cluster around ∼0‰. In order to unravel the cause(s) of the Moon’s unique chlorine isotope signature, we performed a comprehensive study of high-precision in situ Cl isotope measurements of apatite from a suite of Apollo samples with a range of geochemical characteristics and petrologic types. The Cl-isotopic compositions measured in lunar apatite in the studied samples display a wide range of δ37Cl values (reaching a maximum value of +36‰), which are positively correlated with the amount of potassium (K), Rare Earth Element (REE) and phosphorous (P) (KREEP) component in each sample. Using these new data, integrated with existing H-isotope data obtained for the same samples, we are able to place these findings in the context of the canonical lunar magma ocean (LMO) model. The results are consistent with the urKREEP reservoir being characterised by a δ37Cl ∼+30‰. Such a heavy Cl isotope signature requires metal-chloride degassing from a Cl-enriched urKREEP LMO residue, a process likely to have been triggered by at least one large crust-breaching impact event that facilitated the transport and exposure of urKREEP liquid to the lunar surface.

Published
2016
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4. Response-Cretaceous Extinctions

Author

Richard A. F. Grieve, Penny Barton, Arthur R. Sweet, Robert P. Speijer, Peter Schulte, Vivi Vajda, Michael T. Whalen, David A. Kring, Timothy J. Bralower, Alessandro Montanari, Wolfgang Kiessling, Charles S. Cockell, Eric Robin, Joanna Morgan, Clive R. Neal, Elisabetta Pierazzo, Gail L. Christeson, Ignacio Arenillas, Kenneth G. MacLeod, Kirk R. Johnson, Sean P. S. Gulick, Jay Melosh, J.M. Grajales-Nishimura, Tobias Salge, Gareth S. Collins, Greg Ravizza, Jaime Urrutia-Fucugauchi, Takafumi Matsui, Kazuhisa Goto, Richard D Norris, Tamara J. Goldin, Pi Suhr Willumsen, José A. Arz, Wolf Uwe Reimold, Laia Alegret, Philippe Claeys, Christian Koeberl, Paul R. Bown, Alexander Deutsch, Mario Rebolledo-Vieyra, GeoZentrum Nordbayem, Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Departamento de Ciencias de la Tierra, University of Zaragoza - Universidad de Zaragoza [Zaragoza], Department of Earth Sciences [Cambridge, UK], University of Cambridge [UK] (CAM), Department of Earth Sciences [UCL london], University College of London [London] (UCL), Department of Geosciences, Pennsylvania State University (Penn State), Penn State System-Penn State System, Institute of Geophysics [Austin] (IG), University of Texas at Austin [Austin], Earth System Science Group [Brussels] (ESSc), Vrije Universiteit Brussel (VUB), Planetary and Space Sciences Research Institute [Milton Keynes] (PSSRI), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), Department of Lithospheric Research [Wien], Universität Wien, Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Instituto Mexicano del Petróleo (IMP), Earth Sciences Sector, Natural Resources Canada (NRCan), Research and Collections Division, Denver, Denver Museum of Nature and Science, Museum für Naturkunde [Berlin], Center for Lunar Science and Exploration [Houston], Lunar and Planetary Institute [Houston] (LPI), Department of Geological Sciences, University of Missouri [Columbia] (Mizzou), University of Missouri System-University of Missouri System, Earth and Atmospheric, Purdue University [West Lafayette], Osservatorio Geologico di Coldigioco (OGC), Department of Civil and Environmental Engineering and Earth Science [Notre Dame] (CEEES), University of Notre Dame [Indiana] (UND), SIO Geological, Scripps Institution of Oceanography, Planetary Science Institute [Tucson] (PSI), Department of Geology and Geophysics, University of Hawai‘i [Mānoa] (UHM), Unidad de Ciencias del Agua, Centro de Investigación Científica de Yucatán, Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Bruker Nano GmbH, Bruker Nano, Department of Earth and Environmental Sciences [Leuven] (EES), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Geological Survey of Canada [Calgary] (GSC Calgary), Geological Survey of Canada - Office (GSC), Natural Resources Canada (NRCan)-Natural Resources Canada (NRCan), Laboratorio de Paleomagnetismo de Paleomagnetismo y Paleoambientes, Universidad Nacional Autónoma de México (UNAM), Department of Earth and Ecosystem Sciences [Lund], Lund University [Lund], University of Alaska [Anchorage], Universität Erlangen, Université de Zaragoza, University of Cambridge [UK] ( CAM ), Department of Earth Sciences, University College of London [London] ( UCL ), PennState University [Pennsylvania] ( PSU ), Institute for Geophysics, Earth System Science, Vrije Universiteit [Brussel] ( VUB ), Planetary and Space Sciences Research Institute [Milton Keynes] ( PSSRI ), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] ( CEPSAR ), The Open University [Milton Keynes] ( OU ) -The Open University [Milton Keynes] ( OU ), Department of Earth Science and Engineering [London], Westfälische Wilhelms-Universität Münster ( WWU ), Planetary Exploration Research Center, Chiba Institute of Technology ( CIT ), Programa de Geología de Exploracíon y Explotacíon, Instituto Mexicano del Petroleo, Natural Resources Canada, Museum für Naturkunde, Humboldt Universität zu Berlin, Center for Lunar Science and Exploration, Lunar and Planetary Institute [Houston] ( LPI ), UNIVERSITY OF MISSOURI, Osservatorio Geologico di Coldigioco, Department of Civil Engineering and Geological Sciences, University of Notre Dame, Planetary Science Institute [Tucson] ( PSI ), University of Hawaii at Manoa ( UHM ), LAboratoire de Recherche en Mécanique Appliquée ( LARMAUR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] ( LSCE ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Department of Earth and Environmental Sciences, Katholieke Universiteit Leuven ( KU Leuven ), Ressources Naturelles Canada, Universidad Nacional Autónoma de México ( UNAM ), Department of Earth and Ecosystem Sciences, University of Alaska, Penn State Department of Geosciences, Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Scripps Institution of Oceanography (SIO - UC San Diego), University of California [San Diego] (UC San Diego), University of California (UC)-University of California (UC)-University of California [San Diego] (UC San Diego), University of California (UC)-University of California (UC), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM)

Subjects
Extinction event, Sea level change, Multidisciplinary, Extinction, 010504 meteorology & atmospheric sciences, [SDE.MCG]Environmental Sciences/Global Changes, 010502 geochemistry & geophysics, 01 natural sciences, Cretaceous, Paleontology, [ SDE.MCG ] Environmental Sciences/Global Changes, Impact crater, Asteroid, [SDU.STU.CL]Sciences of the Universe [physics]/Earth Sciences/Climatology, Flood basalt, [ SDU.STU.CL ] Sciences of the Universe [physics]/Earth Sciences/Climatology, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The Letters by Archibald et al. , Keller et al. , and Courtillot and Fluteau question our conclusion that the Cretaceous-Paleogene mass extinction was caused by the asteroid impact at Chicxulub. All three Letters stress that Deccan flood basalt volcanism played a major role in the extinction. Keller

Published
2010
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