A transmission electron microscopy (TEM) investigation of opaque phases in shocked chondrites     

Pascal Joreau  Hugues Leroux  Jean-Claude Doukhan 《Meteoritics & planetary science》1996,31(2):305-312

Abstract— Shock defects in the most common silicate minerals of chondrites (olivine, pyroxenes and feldspars) have been investigated in detail, but there have been almost no studies of the shock defects in other components, like metal and sulfide. This probably stems from the fact that these latter phases are opaque in the optical microscope. The same reason explains why veins and melt pockets, which are constituted of microcrystalline or glassy phases (i.e., isotropic) are also poorly documented. We have investigated such phases by analytical transmission electron microscopy (ATEM) in two shocked chondrites, Tenham (L6) and Gaines County (H5). We have characterized shock defects in troilite very similar to those occurring in silicates (i.e., a mosaic texture and sets of straight and very narrow, ?10 nm, lamellae of amorphized FeS). There are many small regions in shocked chondrites that are composed of very fine grained (?1 μm) mixtures of metal and sulfide or of various silicates. They must result from local melting followed by a rapid cooling that prevented grain growth. We have determined the chemical compositions and the volume proportions of the tiny grains in these veins and melt pockets, which has allowed their temperature and pressure (T, P) history to be partially deciphered. Finally, we have observed a dense network of very narrow fractures (down to 10 nm) in the olivine and enstatite grains. These fractures are systematically filled with an amorphous (or cryptocrystalline) material that stems from the melt pockets and was injected when the fractures were opened by the rarefaction wave. This material was then quenched at the contact with the colder crystalline rims.  相似文献   

Experimental study and TEM characterization of dusty olivines in chondrites: Evidence for formation by in situ reduction     

Hugues Leroux  Guy Libourel  Laurence Lemelle  Fran&#x;ois Guyot 《Meteoritics & planetary science》2003,38(1):81-94

Abstract— An analytical transmission electron microscopy (ATEM) study was undertaken in order to better understand the formation conditions of dusty olivines (i.e., olivines containing abundant tiny inclusions of Fe‐Ni metal) in primitive meteorites. Dusty olivines from type I chondrules in the Bishunpur chondrite (LL3.1) and from synthetic samples obtained by reduction of San Carlos olivines were examined. In both natural and experimental samples, micron size metal blebs observed in the dusty region often show preferential alignments along crystallographic directions of the olivine grains, have low Ni contents (typically <2 wt%), and are frequently surrounded by a silica‐rich glass layer. These features suggest that dusty olivines are formed by a sub‐solidus reduction of initially fayalitic olivines according to the following reaction: Some volatilization of SiO_gas may account for the apparent excess of metal relative to silica‐rich glass observed in both experimental and natural samples. Comparison with experimentally produced dusty olivines suggests that time scales of the order of minutes usually inferred for chondrule formation are also adequate for the formation of dusty olivines. These observations are in agreement with the hypothesis that at least part of the metal phase in chondrites originated from reduction during chondrule formation.  相似文献   

Synthesis of magnitude and focal mechanism computations for the M ≥ 4.5 earthquakes in France for the period 1995–2000     

Hugues Dufumier 《Journal of Seismology》2002,6(2):163-181

This paper proposes a synthesis of thestudies made in terms of source parametersevaluation for the last earthquakes oflocal magnitude greater than 4.5 whichoccurred in or nearby France during thelast five years. Focal mechanisms andseismic moments have been computed for thethree most important events, largely feltby the population: St Paul de Fenouillet(February 18^th 1996, M_L 5.6),Annecy-Epagny (July 15^th 1996, M_L5.2) and St-Béat (October 4^th1999, M_L 4.8). These focal mechanismshave been obtained either by regionalmoment tensor inversion or from firstmotion polarities and are compared withcomplementary studies made on theseearthquakes. In addition, for the otherearthquakes of local magnitude greater than4.5 which occurred nearby French borderssince the beginning of the recording ofbroadband data by the RéNaSS(Réseau National de SurveillanceSismique, French Seismological Survey) inmid–1995, several magnitude calculationsconcerning the following earthquakes arepresented: Pamplona (25/2/1996, M_L4.7), Aoste (31/03/1996, M_L 4.6),Imperia (24/2/1997, M_L 4.5),Barcelonette (31/10/1997, M_L 4.8),Pamplona (27/10/1998, M_L 4.9), andBonifacio (26/4/2000, M_L 4.5). Localmagnitudes are usually higher thanthe M_b magnitudes reported by the PDE(Preliminary Determination of Epicenters),while the extension of the Msz scale toregional magnitudes and the Mw magnitudesderived from seismic moments give smallervalues. The relative importance of thevarious earthquakes in terms of surfacewave magnitude or seismic moment does notalways agree with that implied by localmagnitudes.  相似文献   

Estimations of mercury fluxes emitted by Mount Etna Volcano     

H. Dedeurwaerder  G. Decadt  W. Baeyens 《Bulletin of Volcanology》1982,45(3):191-196

A sampling and measuring device which enables the assessment of atmospheric particulate and gaseous mercury concentrations has been tested on Mount Etna Volcano. Particulate matter is collected on a Whatman GF/C of 1.0 µm pore-size, gaseous mercury species on a Au-column. The analysis is carried out in two steps: (1) the mercury species collected on the filter or the Au-column are transferred to a fixed analytical Au-column; (2) mercury liberated from this column during the second step is detected with a Mercury Vapour Monitor. Average concentrations of gaseous and particulate mercury in ambient sampling sites on Mount Etna are 3.8 ng m^?3 and 0.49 ng m^?3 respectively. Average concentrations of gaseous and particulate mercury in the plume of Bocca Nuova on Mount Etna are 15 ng m^?3 and 24 ng m^?3 respectively. An estimation of the total mercury discharge from Mount Etna amounts to 2.5 10^?2 tons day^?1.  相似文献   

Borehole-guided AVO analysis of P-P and P-S reflections: Quantifying uncertainty on density estimates     

Hugues A. Djikpesse  Wael Meghirbi  Irina Nizkous  Di Cao 《Geophysical Prospecting》2006,54(5):515-523

Seismic properties of isotropic elastic formations are characterized by the three parameters: acoustic impedance, Poisson's ratio and density. Whilst the first two are usually well estimated by analysing the amplitude variation with angle (AVA) of reflected P‐P waves, density is known to be poorly resolved. However, density estimates would be useful in many situations encountered in oil and gas exploration, in particular, for minimizing risks in looking ahead while drilling. We design a borehole seismic experiment to investigate the reliability of AVA extracted density. Receivers are located downhole near the targeted reflectors and record reflected P‐P and converted P‐S waves. A non‐linear, wide‐angle‐based Bayesian inversion is then used to access the a posteriori probability distributions associated with the estimation of the three isotropic elastic parameters. The analysis of these distributions suggests that the angular variation of reflected P‐S amplitudes provides additional substantial information for estimating density, thus reducing the estimate uncertainty variance by more than one order of magnitude, compared to using only reflected P‐waves.  相似文献   

A TEM study of exsolution in Ca-rich pyroxenes from the Paris and Renazzo chondrites: Determination of type I chondrule cooling rates     

Priscille Cuvillier  Noël Chaumard  Hugues Leroux  Brigitte Zanda  Roger H. Hewins  Damien Jacob  Bertrand Devouard 《Meteoritics & planetary science》2018,53(3):482-492

We conducted a transmission electron microscope study of the exsolution microstructures of Ca-rich pyroxenes in type I chondrules from the Paris CM and Renazzo CR carbonaceous chondrites in order to provide better constraints on the cooling history of type I chondrules. Our study shows a high variability of composition in the augite grains at a submicrometer scale, reflecting nonequilibrium crystallization. The microstructure is closely related to the local composition and is thus variable inside augite grains. For compositions inside the pyroxene miscibility gap, with a wollastonite (Wo) content typically below 40 mole%, the augite grains contain abundant exsolution lamellae on (001). For grain areas with composition close to Wo₄₀, a modulated texture on (100) and (001) is the dominant microstructure, while areas with compositions higher than Wo₄₀ do not show any exsolution microstructure development. To estimate the cooling rate, we used the spacing of the exsolution lamellae on (001), for which the growth is diffusion controlled and thus sensitive to the cooling rate. Despite the relatively homogeneous microstructures of augite grains with Wo < 35 mole%, our study of four chondrules suggests a range of cooling rates from ~10 to ~1000 °C h⁻¹, within the temperature interval 1200–1350 °C. These cooling rates are comparable to those of type II chondrules, i.e., 1–1000 °C h⁻¹. We conclude that the formation of type I and II chondrules in the proto-solar nebula was the result of a common mechanism.  相似文献   

Consistent past half-century trends in the atmosphere, the sea ice and the ocean at high southern latitudes     

Hugues Goosse  Wouter Lefebvre  Anne de Montety  Elisabeth Crespin  Alejandro H. Orsi 《Climate Dynamics》2009,33(7-8):999-1016

Simulations performed with the climate model LOVECLIM, aided with a simple data assimilation technique that forces a close matching of simulated and observed surface temperature variations, are able to reasonably reproduce the observed changes in the lower atmosphere, sea ice and ocean during the second half of the twentieth century. Although the simulated ice area slightly increases over the period 1980–2000, in agreement with observations, it decreases by 0.5 × 10⁶ km² between early 1960s and early 1980s. No direct and reliable sea ice observations are available to firmly confirm this simulated decrease, but it is consistent with the data used to constrain model evolution as well as with additional independent data in both the atmosphere and the ocean. The simulated reduction of the ice area between the early 1960s and early 1980s is similar to the one simulated over that period as a response to the increase in greenhouse gas concentrations in the atmosphere while the increase in ice area over the last decades of the twentieth century is likely due to changes in atmospheric circulation. However, the exact contribution of external forcing and internal variability in the recent changes cannot be precisely estimated from our results. Our simulations also reproduce the observed oceanic subsurface warming north of the continental shelf of the Ross Sea and the salinity decrease on the Ross Sea continental shelf. Parts of those changes are likely related to the response of the system to the external forcing. Modifications in the wind pattern, influencing the ice production/melting rates, also play a role in the simulated surface salinity decrease.  相似文献   

A TEM study of four particles extracted from the Stardust track 80     

Julien Stodolna  Damien Jacob  Hugues Leroux 《Meteoritics & planetary science》2009,44(10):1511-1518

Abstract— Four particles extracted from track 80 at different penetration depths have been studied by analytical transmission electron microscopy (ATEM). Regardless of their positions within the track, the samples present a comparable microstructure made of a silica rich glassy matrix embedding a large number of small Fe‐Ni‐S inclusions and vesicles. This microstructure is typical of strongly thermally modified particles that were heated and melted during the hypervelocity impact into the aerogel. X‐ray intensity maps show that the particles were made of Mg‐rich silicates (typically 200 nm in diameter) cemented by a fine‐grained matrix enriched in iron sulfide. Bulk compositions of the four particles suggest that the captured dust particle was an aggregate of grains with various iron sulfide fraction and that no extending chemical mixing in the bulb occurred during the deceleration. The bulk S/Fe ratios of the four samples are close to CI and far from the chondritic meteorites from the asteroidal belt, suggesting that the studied particles are compatible with chondritic‐porous interplanetary dust particles or with material coming from a large heliocentric distance for escaping the S depletion.  相似文献   

Weathering features in shocked quartz from the Ries impact crater,Germany     

Hugues Leroux 《Meteoritics & planetary science》2005,40(9-10):1347-1352

Abstract— Shocked quartz from the ejecta of the Ries impact structure has been investigated by analytical transmission electron microscopy (ATEM). Quartz grains display numerous planar fractures (PFs) and planar deformation features (PDFs). Both are partly or fully replaced by a mineral of the kaolinite group (likely halloysite). Its formation involves fluid circulation into the dense fracture networks, dissolution and removal of the amorphous phase initially present in PDFs, and finally, precipitation and crystallization of the kaolinite group mineral from solutions resulting from the chemical alteration of adjacent minerals (feldspars and biotite). Kaolinite group minerals are typical of hydrothermal alteration at low temperature, in humid climate, and under moderately acid conditions and, thus, this alteration may not be directly related to the impact event itself. However, the weathering features were strongly enhanced by the shock‐generated microstructure, in particular by fractures that provided pathways for fluid circulation.  相似文献   

Pyroxene microstructure in the Northwest Africa 856 martian meteorite     

Hugues Leroux  Bertrand Devouard  Patrick Cordier  Franois Guyot 《Meteoritics & planetary science》2004,39(5):711-722

Abstract— Transmission electron microscopy was used to examine pyroxene microstructure in the Northwest Africa (NWA) 856 martian meteorite to construct its cooling and shock histories. All pyroxenes contain strained coherent pigeonite/augite exsolution lamellae on (001). The average width and periodicity of lamellae are 80 and 400 nm, respectively, indicating a cooling rate below 0.1 °C/hr for the parent rock. Pigeonite and augite are topotactic, with strained coherent interfaces parallel to (001). The closure temperature for Ca‐Fe, Mg interdiffusion, estimated from the composition at the augite pigeonite interface, is about 700 °C. Tweed texture in augite reveals that a spinodal decomposition occurred. Locally, tweed evolved toward secondary pigeonite exsolutions on (001). Due to the decreasing diffusion rate with decreasing temperature, “M‐shaped” concentration profiles developed in augite lamellae. Pigeonite contains antiphase boundaries resulting from the C2/c to P2₁/c space group transition that occurred during cooling. The reconstructive phase transition from P2₁/c clinopyroxene to orthopyroxene did not occur. The deformation (shock) history of the meteorites is revealed by the presence of dislocations and mechanical twins. Dislocations are found in glide configuration, with the [001](100) glide system preferentially activated. They exhibit strong interaction with the strained augite/pigeonite interfaces and did not propagate over large distances. Twins are found to be almost all parallel to (100) and show moderate interaction with the augite/pigeonite interfaces. These twins are responsible for the plastic deformation of the pyroxene grains. Comparison with microstructure of shocked clinopyroxene (experimentally or naturally shocked) suggests that NWA 856 pyroxenes are not strongly shocked.  相似文献