Making tissintite: Mimicking meteorites in the multi-anvil

1Melinda J. Rucks, 1,2Matthew L. Whitaker, 1Timothy D. Glotch,1,2 John B. Parise, 1Steven J. Jaret, 1Tristan Catalano, 3M. Darby Dyar
American Mineralogist 103, 1516-1519 Link to Article [https://doi.org/10.2138/am-2018-6539]
1Department of Geosciences, Stony Brook University, Stony Brook, New York 11794-2100, U.S.A.
2Mineral Physics Institute, Stony Brook University, Stony Brook, New York 11794-2100, U.S.A
3Department of Astronomy, Mount Holyoke College, South Hadley, Massachusetts 01075, U.S.A.
Copyright: The Mineralogical Society of America

Tissintite is a shock-induced, Ca-rich mineral, isostructural to jadeite, observed in several meteorite samples such as the martian shergottite Tissint. It may form within a “Goldilocks Zone,” indicating a potential to provide strict constraints on peak pressure and temperature conditions experienced during impact. Here we present the first laboratory synthesis of tissintite, which was synthesized using a large volume multi-anvil apparatus at conditions ranging from 6–8.5 GPa and 1000–1350 °C. For these experiments, we utilized a novel heating protocol in which we reached impact-relevant temperatures within 1 s and in doing so approximated the temperature-time conditions in a post-shock melt. We have established that heating for impact-relevant timescales is not sufficient to completely transform crystalline labradorite to tissintite at these pressures. Our findings suggest that tissintite forms from amorphous plagioclase during decompression.

Vestaite, (Ti4+Fe2+)Ti3 4+O9, a new mineral in the shocked eucrite Northwest Africa 8003

1,2Run-Lian Pang, 2Dennis Harries, 2Kilian Pollok, 1Ai-Cheng Zhang, 2,3Falko Langenhorst
American Mineralogist 103, 1502-1511 Link to Article [https://doi.org/10.2138/am-2018-6522]
1State Key Laboratory for Mineral Deposits Research, School of Earth Sciences and Engineering, Nanjing University, Nanjing 210046, China
2Institute of Geosciences, Friedrich Schiller University Jena, D-07745 Jena, Germany
3Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai’i at Manoa, Honolulu, Hawaii 96822, U.S.A.
Copyright: The Mineralogical Society of America

Our investigations on the shocked eucrite Northwest Africa (NWA) 8003 revealed the occurrence of a new mineral, vestaite [IMA 2017-068;(Ti4+Fe2+)Ti3 4+O9]. This mineral coexists with corundum, ilmenite, and Al-Ti-rich pyroxene in shock melt pockets. It has an empirical chemical formula of
(Ti0.73 4+ Fe0.63 2+Al0.60Mn0.03Mg0.02Cr0.01)Ti3 4+O9
and the monoclinic C2/c structure of schreyerite. The ideal vestaite structure can be considered as a modular structure with an alternate intergrowth of M3O5-type (M = Ti4+,Fe2+,Al) and Ti2O4-type slabs. Alternatively, it can also be envisaged as a crystallographic shear structure with periodically shearing of rutile or α-PbO2 units. Streaking and splitting of diffraction spots observed in selected-area electron diffraction patterns indicate planar defects in the modular structure of vestaite. Our observations reveal that vestaite crystallized at high pressure (≤10 GPa) from a melt that represents a mixture of ilmenite and silicate components. A robust constraint on its formation conditions and stability field cannot yet be provided due to the lack of experimental data for these systems. Vestaite is a new, shock-generated mineral first found in a meteorite of the howarditeeucrite-diogenite (HED) clan, the largest achondrite group. Its discovery is not only of significance to the meteoritic mineralogy, but it could also be of interest to materials science.

Temperature constraints by Raman spectroscopy of organic matter in volatile-rich clasts and carbonaceous chondrites

1Robbin Visser, 1Timm John, 1Martina Menneken, 2Markus Patzek, 2Addi Bischoff
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.08.037]
1Freie Universität Berlin, Institut für Geologische Wissenschaften, Malteserstr. 74-100, 12249 Berlin
2Institut für Planetologie, WWU Münster, Wilhelm-Klemm-Str. 10, D-48149 Münster, Germany
Copyright Elsevier

An important question regarding the formation of the solar system is how planetary bodies developed from dust and ice into the planets and planetary bodies. A particularly interesting topic is the thermal evolution of carbonaceous chondrites and volatile-rich clasts that could have originated from CM- and CI-like parent bodies. Two types of these volatile-rich clasts, which are a particular type of dark clasts, can be found. These clasts are mineralogically very similar to CM and CI chondrites and can occasionally be found in achrondritic meteorites. Mineral assemblages suggest that both CM and CI chondrites as well as volatile-rich clasts experienced low peak temperatures. However, these mineral assemblages only offer large estimated temperature ranges to describe the thermal history of CM and CI chondrites, and the thermal history of volatile-rich clasts has not been previously described. In this study, to gain a better understanding of the thermal history of both CM and CI chondrites and volatile-rich clasts, we estimated peak temperatures of 30 volatile-rich clasts (16 CI-, and 14 CM-like) in 10 different host meteorites (4 polymict ureilites, 5 polymict eucrites and 1 howardite) by Raman carbon thermometry. An automated method was developed in order to describe over 4000 collected Raman spectra using four pseudovoigt functions. The full width half maximum (FWHM) of the D1-band was then used to calculate peak temperatures. Results were then compared to Raman data of 8 different well-studied carbonaceous chondrites (including CI and CM chondrites) to evaluate the suggestion that volatile-rich clasts are composed of similar material to the equivalent CI and CM chondrites. Our results show that the peak temperatures experienced by CI-like clasts range between 30-110 °C with an average of about 65 ± 25 °C; the peak temperatures experienced by CM-like clasts range from 50-110 °C with an average of about 70 ± 25 °C. Six of the 8 studied carbonaceous chondrites (CM, CI, CR or C2ungr) also plot in the same low-temperature range between 50 °C and 75 °C and can thus be considered to have formed under similar temperature conditions as the volatile-rich clasts. This is in agreement with previous suggestions, based on their mineral compositions that volatile-rich clasts and CI and CM carbonaceous chondrites are composed of similar materials. The peak temperatures for carbonaceous chondrites determined in this study considerably reduce the range of temperature estimates proposed previously for these chondrites by different methods. By highlighting the ability of our methodology to evaluate data in an automated way, this study shows that Raman carbon thermometry is a good analytical technique for obtaining information about peak temperatures in small and delicate samples.

Prevalence and nature of heating processes in CM and C2-ungrouped chondrites as revealed by insoluble organic matter

1E.Quirico et al. (>10)
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.08.029]
1University Grenoble Alpes, CNRS, Institut de Planétologie et Astrophysique de Grenoble (IPAG), UMR 5274, Grenoble F-38041, France
Copyright Elsevier

Chondrites are exhumed from their parent bodies by impacts, which at the same time can result in heating and mechanical modification (compaction, deformation, fracturing, etc.). However, whether impacts are responsible for the occurrence of heated C2s remains controversial since radiogenic and solar heating have also been invoked to explain them. Here we report a Raman and infrared study of the composition and structure of Insoluble Organic Matter (IOM) in a series of 39 CM and C2-ungrouped chondrites. These parameters are tracers of the extent and nature of thermal metamorphism a meteorite has experienced and reflect the degree to which the thermally driven and irreversible carbonization of IOM has proceeded. We propose a carbon-based classification of heated C2 chondrites that reveals a high occurrence frequency of thermally processed C2 chondrites (> 36 %). This classification is in agreement with the mineralogical classification scheme of [Nakamura (2005) Post-hydration thermal metamorphism of carbonaceous chondrites. J. Mineral. Petrol. Sci. 100, 260–272]. Strongly heated C2 chondrites (PCA 02012, PCA 91008, Y 96720) display an IOM structural evolution that is dissimilar to that of type 3 chondrites that experienced long duration radiogenic thermal metamorphism. These differences almost certainly reflect kinetic constraints on IOM modification during short duration heating events. QUE 93005 is a weakly heated chondrite that experienced a retrograde aqueous alteration. Its very aliphatic-rich IOM points to a parent body hydrogenation through interactions with water. The closed-system conditions required by this mechanism could be satisfied by a kinetic confinement during a very short duration impact. MET 01072, a heavily compacted and uni-axially deformed chondrite, did not experience post-accretional heating. In this case, the deformation features probably reflect a low-velocity impact. In contrast, the weakly metamorphosed chondrite EET 96029 experienced one or several low pressure impacts that triggered mild heating and partial dehydration without deformation features. The study of a series of lithologies from the Tagish Lake C2-ungrouped chondrite confirms the coexistence of various degrees of post-accretional alteration, the most altered lithologies having experienced a moderate degree of heating. Overall, the high prevalence of heating in C2 chondrites, the evidence of short-duration heating in the most heated C2s and the ability of low velocity collisions to trigger heating favor impacts (against solar heating), as the dominant heating mechanism. Finally, our set of data does not support the action of a low temperature oxidation process that would control the aliphatic abundance in unheated primitive C2s.

Seconds after impact: Insights into the thermal history of impact ejecta from diffusion between lechatelierite and host glass in tektites and experiments

1Catherine A.Macris, 1Paul D.Asimow, 2James Badro, 1John M.Eiler, 3Youxue Zhang, 1Edward M.Stolper
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.08.031]
1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, 91125, USA
2Institut de Physique du Globe de Paris, Paris, France
3Earth and Environmental Sciences, University of Michigan, Ann Arbor, MI, 48109, USA
Copyright Elsevier

Tektites contain inclusions of lechatelierite, nearly pure SiO2 glass formed by quenching of quartz grains melted during hypervelocity impacts. We report the discovery in a tektite of chemically zoned boundary layers (ca 20 μm) between lechatelierite and host felsic glass. These boundary layers in tektites formed by chemical diffusion between molten silica inclusions (quenched to lechatelierite on cooling) and surrounding felsic melt. We reproduced the details of these boundary layers via experiments on mixtures of powdered natural tektite plus quartz grains heated to 1800-2400 ˚C for 1-120 s using an aerodynamic levitation laser heating furnace. The results of these experiments were used to provide quantitative constraints on possible thermal histories of the natural sample.

The experiments successfully reproduced all major aspects of the concentration profiles from the natural sample including diffusion length scale, strong asymmetry of the concentration profiles with respect to the Matano plane (due to the strong concentration dependence of the diffusivities of all oxides on SiO2 content), similarities in lengths of the diffusive profiles (due to control by the diffusion of SiO2 on the diffusivity of the other oxides), and differences in the shapes of the profiles among the oxides (including a maximum in the diffusion profile of K2O due to uphill diffusion). The characteristic lengths of all non-alkali oxide profiles are proportional to t from which diffusivities and activation energies can be derived; these results are consistent with measurements in melts with lower SiO2 contents and at lower temperatures reported in the literature. We also fit the experimental profiles of SiO2 and Al2O3 using simple formulations of the dependence of their diffusivities on SiO2 content and temperature, yielding results similar to those obtained from the t dependence of the characteristic profile lengths.

The quantitative characterization of diffusion in boundary layers based on our experiments allow us to set limits on the thermal history of the natural tektite in which the boundary layers were discovered. If the interdiffusion between the silica and felsic melts occurred at constant temperature, the duration of heating experienced by the natural tektite we studied depends on temperature; possible solutions include heating at ∼2000 °C for ∼70 s, -2400 °C for ∼3 seconds. We also explored non-isothermal, asymptotic cooling histories; for a maximum temperature of 2400 °C, a characteristic cooling time scale of ∼50 s is implied, whereas, for 2000 °C, the time scale is ∼1400 s. Further, a maximum temperature of ∼2360 °C yields an effective diffusive time scale of ∼5 s, a cooling time scale of ∼90 s, and a cooling rate at the glass transition temperature of ∼5 °C/s; results that are consistent with independent estimates of cooling time scales for ∼1 cm clasts (Xu and Zhang, 2002), as well as cooling rates at the glass transition temperature (Wilding et al., 1996) – thus satisfying all currently available relevant data. More complex T-t paths are possible and can also be modeled using our experimental results and compared with and used as tests of the accuracy of physical models of tektite-forming impact events.

Baddeleyite as a widespread and sensitive indicator of meteorite bombardment in planetary crusts

1,2,3White, L.F., 1Darling, J.R., 4Moser, D.E., 5Cayron, C., 4Barker, I., 1Dunlop, J., 2,3Tait, K.T.
Geology 46, 719-722 Link to Article [DOI: 10.1130/G45008.1]
1School of Earth and Environmental Sciences, University of Portsmouth, Portsmouth, United Kingdom
2Department of Natural History, Royal Ontario Museum, 100 Queens Park, Toronto, ON, Canada
3Deparment of Earth Sciences, University of Toronto, Toronto, ON, Canada
4Department of Earth Sciences, University of Western Ontario, London, Canada
5Laboratory of ThermoMechanical Metallurgy (LMTM), École Polytechnique Fédérale de Lausanne (EPFL), Rue de la Maladière, 71b, Neuchâtel, Switzerland

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Chondrules as direct thermochemical sensors of solar protoplanetary disk gas

1,2Libourel, G., 3Portail, M.
Science Advances 4, eaar3321 Link to Article [DOI: 10.1126/sciadv.aar3321]
1Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, UMR 7293 Lagrange, Boulevard de l’Observatoire, CS34229, Nice Cedex 4, France
2Hawai‘i Institute of Geophysics and Planetology, School of Ocean, Earth Science and Technology, University of Hawai‘i, Mānoa, Honolulu, HI, United States
3Université Côte d’Azur, CNRS–Centre de Recherches sur l’Hétéro-Epitaxie et ses Applications, Sophia Antipolis, Rue Bernard Grégory, Valbonne, France

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Results of mineralogical and petrological research of new samples on the Pułtusk meteorite at the 150th anniversary of the fall [Wyniki badań mineralogicznych i petrologicznych nowych okazów meteorytu Pułtusk w 150 rocznicȩ spadku]

1Przylibski, T.A.,1Łuszczek, K.
Przeglad Geologiczny 66, 368-378 Link to Article [DOI: 10.3390/min8060240]
1Wydział Geoinżynierii, Górnictwa i Geologii, Politechnika Wrocławska, Wybrzeże S. Wyspiańskiego 27, Wrocław, Poland

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Nitrogen abundance and isotope analysis of silicate glasses by secondary ionization mass spectrometry

1Füri, E.,1Deloule, E., 1,2Dalou, C.
Chemical Geology 493, 327-337 Link to Article [DOI: 10.1016/j.chemgeo.2018.06.008]
1Centre de Recherches Pétrographiques et Géochimiques, UMR 7358, CNRS-UL, 15 rue Notre Dame des Pauvres, BP20, Vandoeuvre-lès-Nancy Cedex, France
2University of Minnesota, Department of Earth Sciences, 108 Pillsbury Hall, Minneapolis, MN, United States

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