¹Harry Y.McSweenJr.,²Carol A.Raymond,³Edward M.Stolper,⁴David W.Mittlefehldt,³Michael B.Baker,⁵Nicole G.Lunning,⁶Andrew W.Beck,⁷Timothy M.Hahn
Geochemistry (Chemie der Erde) Link to Article [https://doi.org/10.1016/j.chemer.2019.07.008]
¹Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA
²Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
³Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
⁴NASA Johnson Space Center, Houston, TX 77058, USA
⁵Department of Earth and Planetary Sciences, Rutgers University, Piscataway, NJ 08854, USA
⁶Department of Petroleum Engineering and Geology, Marietta College, Marietta, OH 45750, USA
⁷Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA
Copyright Elsevier

Quantifying the amounts of various igneous lithologies in Vesta’s crust allows the estimation of petrologic ratios that describe the asteroid’s global differentiation and subsequent magmatic history. The eucrite:diogenite (Euc:Diog) ratio measures the relative proportions of mafic and ultramafic components. The intrusive:extrusive (I:E) ratio assesses the effectiveness of magma ascent and eruption. We estimate these ratios by counting numbers and masses of eucrites, cumulate eucrites, and diogenites in the world’s meteorite collections, and by calculating their proportions as components of crustal polymict breccias (howardites) using chemical mixing diagrams and petrologic mapping of multiple thin sections. The latter two methods yield a Euc:Diog ratio of ∼2:1, although meteorite numbers and masses give slightly higher ratios. Surface lithologic maps compiled from spectra of Dawn spacecraft instruments (VIR and GRaND) yield Euc:Diog ratios that bracket estimates of Euc:Diog from the meteorites. The I:E ratios from HEDs lie between 0.5–2.1:1, due to uncertainties in identifying cumulate eucrite. Gravity mapping of Vesta by the Dawn spacecraft supports the existence of diogenite plutons in the crust. Quantifying the proportion of high-density diogenitic crust in the gravity map yields I:E ratios of 0.8-1:2:1, values which are bracketed by calculations based on HEDs. The I:E ratio for Vesta is lower than for Earth and Mars, consistent with physical modeling of asteroid-size bodies. Nevertheless, it indicates a significant role for pluton emplacement during the formation of Vesta’s crust. These results are inconsistent with simple differentiation models that produce the crust by crystallization of a global magma ocean, unless residual melts are extracted into crustal magma chambers.

¹Emily J.Foote,¹David A.Paige,²Michael K.Shepard,³Jeffrey R.Johnson,⁴Stuart Biggar
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2019.113456]
¹University of California Los Angeles, 595 Charles Young Drive East, Box 951567, Los Angeles, CA 90095-1567
²Bloomsburg University, 400 E. Second St., Bloomsburg, PA 17815, Bloomsburg, PA
³Johns Hopkins University Applied Physics Laboratory, 11101 Johns Hopkins Road, 200-W230, Laurel, MD 20723-6005
⁴College of Optical Sciences, University of Arizona, 1630 E. University Blvd., P.O. Box 210094, Tucson, AZ 85721-0094
Copyright Elsevier

We have acquired a comprehensive laboratory bidirectional measurements of Apollo 11 and Apollo 16 lunar soil samples and have successfully fit photometric models to the laboratory data and have determined the solar spectrum averaged hemispheric reflectance as a function of incidence angle. The Apollo 11 (sample 10084) and 16 (sample 68810) soil samples are two representative end member samples from the Moon, dark lunar maria and bright lunar highlands. We used our solar spectrum averaged albedos in a thermal model and compared our model-calculated normal bolometric infrared emission curves with those measured by the LRO Diviner Lunar Radiometer Experiment. We found excellent agreement at the Apollo 11 site, but at the Apollo 16 site, we found that the albedos we measured in the laboratory were 33% brighter than those required to fit the Diviner infrared data. We attribute this difference at Apollo 16 to increased compaction and decreased maturity of the laboratory sample relative to the natural lunar surface, and to local variability in surface albedos at the Apollo 16 field area that are below the spatial resolution of Diviner.

¹Franck Poitrasson,¹Thomas Zambardi,²Tomas Magna,³Clive R.Neal
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.09.035]
¹Laboratoire Géosciences Environnement Toulouse, Centre National de la Recherche Scientifique UMR 5563 – UPS – IRD – CNES, 14-16, avenue Edouard Belin, 31400 Toulouse, France
²Czech Geological Survey, Klarov 3, CZ-11821 Prague 1, Czech Republic
³Department of Civil and Environmental Engineering and Earth Sciences, University of Notre Dame, 156 Fitzpatrick Hall, Notre Dame, IN 46556, USA
Copyright Elsevier

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.

¹Tsuyoshi Iizuka,²Fred Jourdan,^3,4Akira Yamaguchi,⁵Piers Koefoed,¹Yuki Hibiya,¹Kengo T.M.Ito,⁵Yuri Amelin
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.09.034]
¹Department of Earth and Planetary Science, The University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo 113-0033, Japan
²Western Australian Argon Isotope Facility, JdL Center & Department of Applied Geology, Curtin University, Perth, Western Australia 6845, Australia
³National Institute of Polar Research, Tokyo, Japan
⁴Department of Polar Science, School of Multidisciplinary Science, Graduate University for Advanced Sciences, Tokyo, Japan
⁵Research School of Earth Sciences, The Australian National University, Canberra, ACT 2601, Australia
Copyright Elsevier

Eucrites represent samples of mafic crust of the parent body, likely Vesta, and record a complex geologic history involving magmatism, metamorphism, impact processing, and metasomatism. For better understanding of the geologic history, we present combined ²⁰⁷Pb/²⁰⁶Pb and ⁴⁰Ar/³⁹Ar chronology of four basaltic eucrites showing distinct petrologic features: Agoult, an equilibrated eucrite with granulitic textures; Camel Donga, a brecciated equilibrated eucrite enriched in metallic iron; DaG 380, a partially equilibrated monomict eucrite; and NWA 049, a metasomatized polymict eucrite comprising mostly unequilibrated clasts. The ²⁰⁷Pb/²⁰⁶Pb dating in combination with the acid washing technique was applied to pyroxene-rich and plagioclase-rich fractions, while the ⁴⁰Ar/³⁹Ar dating was performed mainly on plagioclase grains using the laser incremental heating method. The Pb isotopic data for acid leaching residues are more radiogenic than those for acid washes, reflecting efficient removal of non-radiogenic Pb components by the acid washing. Among the residues, however, only those of the Agoult and Camel Donga plagioclase-rich fractions yielded isochrons, rather than errorchrons, with ²⁰⁷Pb/²⁰⁶Pb ages of 4532.39 ± 0.87 Ma and 4515.43 ± 0.42 Ma, respectively. The trace element systematics further suggest that these residues essentially represent contaminant oxide minerals such as ilmenite and chromite rather than plagioclase. On the other hand, the Ar isotopic data for Agoult and Camel Donga yielded plateau ages with weighted means of 4494 ± 9 Ma and 3749 ± 25 Ma, in contrast to those for DaG 380 and NWA 049 that did not return any plateau. The ²⁰⁷Pb/²⁰⁶Pb and ⁴⁰Ar/³⁹Ar ages of Agoult are interpreted to reflect the time of the U–Pb and K–Ar system closure during a prolonged thermal metamorphism. By combining the ages reported here and in the literature with the calculated closure temperatures, the cooling rate of Agoult is determined to be 11 ± 2 ˚C/Ma. This cooling rate corresponds to a burial depth of 10–20 km, indicating that granulitic eucrites were originally crystallized near the surface and were subsequently buried and metamorphosed. The ∼20 Ma younger ²⁰⁷Pb/²⁰⁶Pb ages of Camel Donga than Agoult are considered to reflect delayed burial metamorphism in the source region, whereas the plateau ⁴⁰Ar/³⁹Ar age would record the time of an impact causing brecciation and efficient Ar-degassing of the buried crust. Furthermore, the model ²⁰⁷Pb*/²⁰⁶Pb* dates calculated for acid-washed pyroxenes imply that the burial metamorphism of Agoult and DaG 380 were broadly contemporaneous and also that NWA 049 was metasomatized by fluids within the uppermost crust later than 4.4 Ga.

^1,2Jemma Davidson,²Devin L.Schrader,¹Conel M.O’D.Alexander,¹Larry R.Nittler,³Roxane Bowden
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.09.033]
¹Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, Washington DC, 20015-1305, USA
²Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
³Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Road, Washington DC, 20015-1305, USA
Copyright Elsevier

We re-examine the Renazzo-like (CR) chondrite metamorphic trend based on Cr₂O₃ contents of FeO-rich olivine, indicating that it is only appropriate to use such analyses to identify endmembers (i.e., those that have experienced either no detectable heating or significant heating). As such Miller Range (MIL) 090657 appears to have experienced very minimal (if any) thermal processing and is one of the most pristine CR chondrites analyzed to date, while Graves Nunataks 06100 is the most shock-heated CR chondrite studied.

On the basis of bulk H-C-N isotopic compositions, MIL 090657 appears to be of petrological type 2.7. We also report the H-C-N isotopic compositions of extracted insoluble organic matter, in situ chemical compositional data, presolar grain abundances, and a petrologic description of MIL 090657. As a minimally altered CR chondrite of relatively high mass (133.1 g), MIL 090657 provides an invaluable opportunity to perform coordinated, often destructive, analyses on pristine CR chondrite material.

By combining a number of petrographic characteristics (Cr₂O₃-content of ferroan olivine, Co/Ni ratios of Fe,Ni metal, ratios of Fe# in chondrule olivine and low-Ca pyroxene, and the presence of excess silica in chondrule plagioclase) with bulk isotopic compositions, we demonstrate their utility as indicators for determining the relative pristinity/heating of low petrographic (type 1 to 3) chondrites.

^1,3C.J. Renggli,¹A.B. Palm,¹P.L. King,²P. Guagliardo
Journal of Geophysical Research, Planets (in Press) Link to Article [https://doi.org/10.1029/2019JE006045]
¹Research School of Earth Sciences, The Australian National University, Canberra ACT 2601, Australia
²Centre for Microscopy, Characterization and Analysis, University of Western Australia, PerthWA 6009, Australia
³Institute for Mineralogy, University of Münster, Münster,48149, Germany
Published by arrangement with John Wiley & Sons

Basalts are ubiquitous in volcanic systems on several planetary bodies, including the Earth, Mars, Venus and Jupiter’s moon Io, and are commonly associated with sulfur dioxide (SO₂) degassing. We present the results of an experimental study of reactions between SO₂ and basaltic glasses. We examined Fe‐free basalt, and Fe‐bearing tholeiitic and alkali basalts with a range of Fe³⁺/Fe_total (0.05 to 0.79) that encompass the oxygen fugacities proposed for most terrestrial planetary bodies. Tholeiitic and alkali basalts were exposed to SO₂ at 600, 700 and 800 °C for 1 h and 24 h. Surface coatings formed on the reacted basalts; these contain CaSO₄, MgSO₄, Na₂SO₄, Na₂Ca(SO₄)₂, Fe₂O₃, Fe₃O₄, Fe‐Ti‐(Al)‐oxides and TiO₂. Additionally, the SO₂‐basalt reaction drives nucleation of crystalline phases in the substrate to form pyroxenes and possible Fe‐oxides. A silica‐rich layer forms between the substrate and sulfate coatings. More oxidized basalts may readily react with SO₂ to form coatings dominated by large Ca‐sulfate and oxide grains. In less oxidized basalts (NNO‐1.5 to NNO‐5), reactions with SO₂ will form thin, fine‐grained aggregates of sulfates; such materials are less readily detected by spectroscopy and spectrometry techniques. In contrast, in very reduced basalts (lower than NNO‐5), typical of the Moon and Mercury, SO₂ is typically a negligible component in the magmatic gas, and sulfides are more likely.

¹H.M.Sargeant,¹F.A.J.Abernethy,¹S.J.Barber,¹I.P.Wright,¹M.Anand,¹S.Sheridan,¹A.Morse
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104751]
¹The Open University, United Kingdom

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¹Stefan Linke,²Lisa Windisch,³Nico Kueter,⁴Jan Egil Wanvik,¹Anna Voss,¹Enrico Stoll,²Carsten Schilde,²Arno Kwade
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104747]
¹Institute of Space Systems, TU Braunschweig, Hermann-Blenk-Straße 23, 38108 Brauschweig, Germany
²Institute for Particle Technology, TU Braunschweig, Volkmaroder Straße 5, 38104 Braunschweig, Germany
³Institute of Geochemistry and Petrology, Federal Institute of Technology (ETH) Zurich, Clausiusstrasse 25, 8092, Zurich, Switzerland
⁴Geological Survey of Norway, Leiv Eiriksons vei 39, 7040 Trondheim, Norway

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

^1,2Sheng Gou,^1,2,3 Kaichang Di,^1,3Zongyu Yue,¹Zhaoqin Liu,⁴Zhiping He,⁴Rui Xu,⁵Honglei Lin,^1,2Bin Liu,¹Man Peng,¹Wenhui Wan,¹Yexin Wang,⁶Jianzhong Liu
Earth and Planetary Science Letters 528, 115829 Link to Article [https://doi.org/10.1016/j.epsl.2019.115829]
¹State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China
²State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macau, China
³CAS Center for Excellence in Comparative Planetology, Hefei 230026, China
⁴Key Laboratory of Space Active Opto-Electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Science, Shanghai 200083, China
⁵Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
⁶Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550002, China
Copyright Elsevier

China’s Chang’e-4 spacecraft achieved the first ever soft-landing within the South Pole-Aitken (SPA) basin on the farside of the Moon. The Chang’e-4 rover, named Yutu-2, made in-situ spectral observations on lunar regolith and a rock fragment at 11 locations during a nominal three-month mission period. The lunar regolith has a relative high olivine/pyroxene ratio, with the pyroxene being chiefly Mg-rich Low-Ca pyroxene (LCP). The rock fragment has a similar Mg-rich composition to that of the regolith. According to the surrounding topographic and geologic context, though originating from the lower base of a differentiated melt pool cannot be excluded here, the rover observed regolith and rock fragment are very likely to be lunar mantle materials excavated from nearby Finsen crater.

^1,2Toni Schulz,¹Florian Sackl,¹ Elisabeth Fragner,³Ambre Luguet,^3,4David Van Acken,⁵Begosew Abate,⁶Dimitri D.Badjukov,^1,7Christian Koeberl
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2019.08.045]
¹Department of Lithospheric Research, University Vienna, Althanstrasse 14, 1090 Vienna, Austria
²Institut für Geologie und Mineralogie, Universität zu Köln, Zülpicher Strasse 49b, 50674 Köln, Germany
³Steinmann-Institut für Geologie, Mineralogie and Paläontologie, Universität Bonn, Poppelsdorfer Schloss, 53115 Bonn, Germany
⁴Irish Centre for Research in Applied Geosciences (iCRAG), UCD School of Earth Sciences, University College Dublin, Belfield, Dublin 4, Ireland
⁵Orbit Ethiopia PLC, Addis Ababa, Ethiopia
⁶Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Science, 19 Kosygin Str., 119991 Moscow, Russia
⁷Natural History Museum, Burgring 7, 1010 Vienna, Austria
Copyright Elsevier

The Zhamanshin impact structure, which is about 1 Myr old, has a diameter of 14-km and is situated in the semi-arid region of Kazakhstan (48°24’N,60°58’E). It has a heterogeneous suite of target rocks, including predominantly crustal lithologies (e.g., clays and siltstones) with minor ultramafics.
Zhamanshin is known for its unique association of impact glasses, including basic and acidic varieties of zhamanshinites and (tektite-like and few aerodynamically-shaped) irghizites. The origin of both of these impact glasses has long been debated, which is complicated by incomplete sampling of target lithologies at the Zhamanshin site and a limited number of isotopic analyses. However, such studies are a prerequisite for a comprehensive discussion of the mechanisms that formed the unique association of different impact glasses in one impact event.
We present major- and trace element contents, as well as combined Sr-Nd isotope data for target rocks and impact glasses from the Zhamanshin impact structure. These data, for the first time, include Paleogene clays and siltstones from a core drilled in the vicinity of the crater and cutting through all major lithologies. The core samples represent an important source lithology for the impactites from the Zhamanshin area.
Mixing calculations, based on the geochemical data and Sr-Nd isotope signatures, indicate that irghizites and Si-rich zhamanshinites can be produced from variously homogenized mixtures of mainly clays and siltstones with minor additions of ultrabasic rocks. Based on highly siderophile element (HSE) and Os isotope data (including the first analyses of the clay and siltstone lithologies) we calculated a hypothetical Os composition of the irghizite precursor, allowing us to approximate a chondritic admixture to the irghizites of roughly 1% of a chondritic component. This confirms previous suggestions about the amount of extraterrestrial components. A new HSE and Os isotope dataset for five zhamanshinites reveals, on average, crust-like HSE concentrations and Os isotope compositions confirming earlier suggestions of a lack of meteoritic admixtures to these impact glasses.