Aqueous alteration of the Bali CV3 chondrite: evidence from mineralogy, mineral chemistry, and oxygen isotopic compositions     

Keller LP  Thomas KL  Clayton RN  Mayeda TK  DeHart JM  McKay DS 《Geochimica et cosmochimica acta》1994,58(24):5589-5598

A petrographic, geochemical, and oxygen isotopic study of the Bali CV3 carbonaceous chondrite revealed that the meteorite has undergone extensive deformation and aqueous alteration on its parent body. Deformation textures are common and include flattened chondrules, a well-developed foliation, and the presence of distinctive (100) planar defects in olivine. The occurrence of alteration products associated with the planar defects indicates that the deformation features formed prior to the episode of aqueous alteration. The secondary minerals produced during the alteration event include well-crystallized Mg-rich saponite, framboidal magnetite, and Ca-phosphates. The alteration products are not homogeneously distributed throughout the meteorite, but occur in regions adjacent to relatively unaltered material, such as veins of altered material following the foliation. The alteration assemblage formed under oxidizing conditions at relatively low temperatures (<100 degrees C). Altered regions in Bali have higher Na, Ca, and P contents than unaltered regions which suggests that the fluid phase carried significant dissolved solids. Oxygen isotopic compositions for unaltered regions in Bali fall within the field for other CV3 whole-rocks, however, the oxygen isotopic compositions of the heavily altered material lie in the region for the CM and CR chondrites. The heavy-isotope enrichment of the altered regions in Bali suggest alteration conditions similar to those for the petrographic type-2 carbonaceous chondrites.  相似文献   

Carbon isotopic fractionation in lipids from methanotrophic bacteria: relevance for interpretation of the geochemical record of biomarkers   总被引：11，自引：0，他引：11  

Summons RE  Jahnke LL  Roksandic Z 《Geochimica et cosmochimica acta》1994,58(13):2853-2863

Experiments with cultured aerobic methane oxidising bacteria confirm that their biomarker lipids will be significantly depleted in 13C compared to the substrate. The methanotrophic bacteria Methylococcus capsulatus and Methylomonas methanica, grown on methane and using the RuMP cycle for carbon assimilation, show maximum 13C fractionation of approximately 30% in the resultant biomass. In M. capsulatus, the maximum fractionation is observed in the earliest part of the exponential growth stage and decreases to approximately 16% as cells approach stationary phase. This change may be associated with a shift from the particulate form to the soluble form of the methane monooxygenase enzyme. Less than maximum fractionation is observed when cells are grown with reduced methane availability. Biomass of M. capsulatus grown on methanol was depleted by 9% compared to the substrate. Additional strong 13C fractionation takes place during polyisoprenoid biosynthesis in methanotrophs. The delta 13C values of individual hopanoid and steroid biomarkers produced by these organisms were as much as l0% more negative than total biomass. In individual cultures, squalene was 13C-enriched by as much as 14% compared to the triterpane skeleton of bacteriohopaneaminopentol. Much of the isotopic dispersion in lipid metabolites could be attributed to shifts in their relative abundances, combined with an overall reduction in fractionation during the growth cycle. In cells grown on methanol, where there was no apparent effect of growth stage on overall fractionation there were still significant isotopic differences between closely related lipids including a 5.3% difference between the hopane and 3 beta-methylhopane skeletons. Hopane and sterane polyisoprenoids were also 13C-depleted compared to fatty acids. These observations have significant implications for the interpretation of specific compound isotopic signatures now being measured for hydrocarbons and other lipids present in sediments and petroleum. In particular, biomarker lipids produced by a single organism do not necessarily have the same carbon isotopic composition.  相似文献   

The mesothermal gold-lamprophyre association: significance for an accretionary geodynamic setting,supercontinent cycles,and metallogenic processes     

R. Kerrich  D. A. Wyman 《Mineralogy and Petrology》1994,51(2-4):147-172

Summary Archean shoshonitic lamprophyres are cotemporal and cospatial with gold mineralization in the Superior Province of Canada, both being emplaced along translithospheric structures that demark subprovince boundaries. By analogy with geochemically similar Phanerozoic counterparts, the dikes are a product of specific plate interactions rather than a deep asthenosphere plume-initiated event, and their onset in the late-Archean at 2.7 Ga signifies that Phanerozoic style plate-tectonics was operating at this time. Fresh shonshonitic dikes are characterized by normal background gold contents of 3.9 ± 8.1 ppb (l), close to the value of 3.0 ppb for the bulk continental crust, and average abundances of As, Sb, Bi, W, TI, B, Cu, Pb, Zn, and Mo are also close to their values in bulk continental crust. Thus, fresh lamprophyres are not intrinsically enriched either in Au or elements affiliated with gold in mesothermal deposits, and accordingly do not constitute a special source rock. Platinum group element contents (Ir = 0.4 ± 0.58 ppb; Pt = 5.9 ± 26.5, Pd = 5.5 ± 1.8), in conjunction with Cu, Au, and Ni abundances, define approximately flat patterns on primitive mantle-normalized diagrams, consistent with derivation of the alkaline magmas from a depleted mantle source variably enriched by incompatible elements. Comparable abundances and ratios of Pd/Au, Os/Ir, and Ru/Ir in Archean lamprophyres, Archean komatiites, and Gorgona komatiites signify that the Archean and Phanerozoic upper mantle had similar noble metal contents, such that the prolific greenstone belt Au-Ag vein deposits cannot be explained by secular variations in upper mantle Au abundance alone. The lack of covariation between Au and light rare earth elements in lamprophyres rules out mantle metasomatism as a process generating intrinsically Au-rich magmas.Emplacement of the lamprophyres was diachronous from north (2710 Ma) to south (2670 Ma) in the Superior Province, as was the gold mineralization. Both were related to late transpressional tectonics during successive accretions of individual subprovinces. Alkaline magmatism and gold mineralization are temporally and spatially related because they share a common geodynamic setting, but they are otherwise the products of distinct processes. Much of Archean time was devoid of shoshonites and mesothermal gold deposits. The first widespread inception of this duality at 2.71–2.65 Ga in the Superior and Slave Provinces, Canada, and in India and Australia, may reflect one of the first supercontinent aggregations involving accretionary, Cordilleran style tectonics. Giant mesothermal gold provinces and shoshonites recur through time in the Palaeozoic and Mesozoic in this geodynamic setting.

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Die mesothermale Gold-Lamprophyrassoziation und ihre Bedeutung für Akkretionsgeotektonik, Superkontinent-Zyklen und metallogenetische Prozesse

Zusammenfassung Archaische schoschonitische Lamprophyre sind zeitlich und räumich mit Goldmineralisationen in der Superior Provinz Kanadas vergesellschaftet; beide sind an translithosphärische Strukturen, die die Grenzen von Subprovinzen markieren, geknüpft. Ein Vergleich mit geochemisch ähnlichen phanerozoischen Abfolgen weist darauf hin, daß die Gänge eher durch spezifische Platteninteraktions- und nicht durch Hot Spot initiierte asthenosphärische Prozesse entstanden sind. Ihre spät-archaische Alterseinstufung (ca. 2.7 Ga) belegt somit, daß bereits zu dieser Zeit plattentektonische Prozesse, wie sie für das Phanerozoikum typisch sind, funktionierten.Frische schoschonitische Gänge zeigen mit Durchschnittskruste vergleichbare Untergrundgehalte an Gold von 3.9 ± 8.1 ppb (l), Auch die Gehalte an As, Sb, Bi, W, Tl, B, Cu, Pb, Zn und Mo entsprechen Gehalten der durchschnittlichen Erdkruste. Frische Lamprophyre sind daher nicht an Gold bzw. an anderen für mesothermale AuLagerstätten typischen Elementen angereichert und stellen somit keine spezifischen Muttergesteine dar. Die Gehalte an Platingruppen-Elementen (Ir = 0.4 ± 0.58 ppb; Pt = 5.9 ± 26.5; Pd 5.5 ± 1.8) in Verbindung mit der Verteilung von Cu, Au und Ni definieren einen flachen Trend in auf primitiven Mantel normierten Diagrammen, was mit einer Herkunft der alkalischem Magmen aus einer abgereicherten Mantelquelle, die im unterschiedlichen Ausmaß an einzelnen inkompatiblen Elementen angereichert ist, hinweist. Ähnliche Elementverteilungen bzw. verhältnisse von Pd/Au, Os/Ir und Ru/Ir in archaischen Lamprophyren, archaischen Komatiiten und Gorgona-Komatiiten belegen, daß der archaische und phanerozoische obere Mantel ähnliche Gehalte an Edelund Buntmetallen aufweisen. Die Au-Ag Ganglagerstätten in Greenstone Belts können daher nicht ausschließlich mit einer Variation der Au-Gehalte des oberen Erdmantels erklärt werden. Die fehlende Korrelation zwischen Au und den leichten Seltenen Erden in den Lamprophyren schließt mantelmetasomatische Prozesse für die Bildung von Au-reichen Magmen aus.Die Platznahme der Lamprophyre in der Superior Provinz erfolgte zeitgleich von N (2710 Ma) nach S (2670 Ma) mit der Bildung der Goldmineralisationen. Beide stehen mit einer späten transpressionalen Tektonik während der sukzessiven Akkretion einzelner Subprovinzen in Beziehung. Alkalimagmatismus und Goldmineralisationen sind deshalb räumlich und zeitlich vergesellschaftet, weil sie innerhalb desselben geodynamischen Settings gebildet wurden. Sie sind sonst aber Produkte unterschiedlicher Prozesse. Über weite Zeiträume des Archaikums fehlen Schoschonite und mesothermale Goldlagerstätten. Das erste großangelgte Auftreten beider in der Superior und Slave Provinz Kanadas während 2.71-2.65 Ga und in Indien und Australien könnte eine der ersten Superkontinentaggregationen im Stile einer Cordillera-style Akkretionstektonik widerspiegeln. Riesige mesothermale Goldprovinzen und Schoschonite treten während des Paläo- und Mesozoikums immer wieder, gebunden an diese geotektonische Position, in Erscheinung.

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With 7 Figures  相似文献   

Inner part observation of theβ pictoris disk     

R. Ferlet  A. Lecavelier Des Etangs  G. Perrin  A. Vidal-Madjar  F. Sèvre  F. Colas  J. E. Arlot  C. Buil  H. Beust  A. M. Lagrange-Henri  J. Lecacheux  M. Deleuil  C. Gry 《Astrophysics and Space Science》1994,212(1-2):173-180

The inner regions of the circumstellar disk around Pictoris might be dust-free due to a possible planet which may have cleared up dust particles. We present a new observational technique based on the use of an anti-blooming CCD in order to directly image this zone. The structure of the disk is revealed down to 2 arcsec from the star (30 AU). We show that the Pic disk brightness is neutral inV, R, andI _C , but drops down when going inward inB, possibly related to a change in the dust composition. Also, a slight disk asymmetry is present but inverted from the outer to the inner zones.Paper presented at the Conference onPlanetary Systems: Formation, Evolution, and Detection held 7–10 December, 1992 at CalTech, Pasadena, California, U.S.A.  相似文献   

Long,accurate time series measurements of radial velocities of solar-type stars     

R. S. Mcmillan  T. L. Moore  M. L. Perry  P. H. Smith 《Astrophysics and Space Science》1994,212(1-2):271-280

We have been measuring changes in the radial velocities (RV's) of solar-type stars to search for gravitational perturbations by planets. We transmit violet starlight through a Fabry-Perot etalon interferometer and sense changes in Doppler shift from changes in the fluxes of light on the slopes of stellar absorption lines. Our data now span 6 years. Our observations of the Sun showed earlier that both our technique and the profiles of solar photospheric violet absorption lines can be stable enough to reveal planetary perturbations. We now carry this validation to the spectra of other near-solar-type stars. Annual averages of our RV's of Draconis and Virginis are stable to ±6 m s^–1. The slope of our five-year series of RV's of Bootis A is consistent with the star's well-determined visual astrometric orbit about Bootis B. The Fabry-Perot technique of Doppler shift measurement is fully capable of detecting perturbations due to planets with masses and orbits similar to those of Jupiter.Paper presented at the Conference onPlanetary Systems: Formation, Evolution, and Detection held 7–10 December, 1992 at CalTech, Pasadena, California, U.S.A.  相似文献   

Wind variability in intermediate luminosity B supergiants     

D. Massa  A. Fullterton  R. Prinja 《Astrophysics and Space Science》1994,221(1-2):77-85

We discuss wind variability in intermediate luminosity B supergiants. Because these are not the hottest, most luminous or just about other kind of -est stars, they have not attracted much attention. However, since their wind lines are well-developed, but unsaturated, they make ideal diagnostics for time dependent wind studies. We show that their wind profiles undergo large scale variability and that this phenomenon is quite common. We also discuss a time series for the B0.5 Ib HD 64760 which suggests the long sought after connection between wind and photospheric activity. Newly developed analysis techniques needed to extract physical information from the wind lines are discussed, and results are applied to the time series.  相似文献   

A coronal loop model for the production of X-ray and radio flares in the RS CVn binary HR 1099     

D. F. Falla  L. M. Bartlett  M. H. L. Smith  R. R. Hillier 《Astrophysics and Space Science》1994,211(1):115-126

The RS CVn binary stellar system HR 1099 is a source of both X-ray and radio flares. We present here a model of the system in which the two types of flare are produced by the same population of mildly-relativistic ( 10) electrons, injected into a coronal loop. After reviewing possible radiation mechanisms we conclude that, given the probable conditions in the flaring region, the radio emission is gyrosynchrotron radiation and the X-ray emission is thermal bremsstrahlung. The thermal X-ray source must lie in the stellar chromosphere, but the apparent absence of plasma absorption at radio frequencies indicates that the radio source is located high in the coronal loop. Using the relationships given by Dulk and Marsh (1982) for the radio emission from a power-law electron energy spectrum,N() ( - 1)^–, we conclude that 3 7, with 30% of the electron population trapped in the radio source. Some implications of these results for one particular version of the model are discussed.  相似文献   

A photochemical model of the martian atmosphere     

Nair H  Allen M  Anbar AD  Yung YL  Clancy RT 《Icarus》1994,111(1):124-150

The factors governing the amounts of CO, O2, and O3 in the martian atmosphere are investigated using a minimally constrained, one-dimensional photochemical model. We find that the incorporation of temperature-dependent CO2 absorption cross sections leads to an enhancement in the water photolysis rate, increasing the abundance of OH radicals to the point where the model CO abundance is smaller than observed. Good agreement between models and observations of CO, O2, O3, and the escape flux of atomic hydrogen can be achieved, using only gas-phase chemistry, by varying the recommended rate constants for the reactions CO + OH and OH + HO2 within their specified uncertainties. Similar revisions have been suggested to resolve discrepancies between models and observations of the terrestrial mesosphere. The oxygen escape flux plays a key role in the oxygen budget on Mars; as inferred from the observed atomic hydrogen escape, it is much larger than recent calculations of the exospheric escape rate for oxygen. Weathering of the surface may account for the imbalance. Quantification of the escape rates of oxygen and hydrogen from Mars is a worthwhile objective for an upcoming martian upper atmospheric mission. We also consider the possibility that HOx radicals may be catalytically destroyed on dust grains suspended in the atmosphere. Good agreement with the observed CO mixing ratio can be achieved via this mechanism, but the resulting ozone column is much higher than the observed quantity. We feel that there is no need at this time to invoke heterogeneous processes to reconcile models and observations.  相似文献   

Rate constants for the reactions of the NO3 radical with HCOOH/HCOO− and CH3COOH/CH3COO− in aqueous solution between 278 and 328 K     

M. Exner  H. Herrmann  R. Zellner 《Journal of Atmospheric Chemistry》1994,18(4):359-378

The kinetics of the aqueous phase reactions of NO₃ radicals with HCOOH/HCOO^– and CH₃COOH/CH₃COO^– have been investigated using a laser photolysis/long-path laser absorption technique. NO₃ was produced via excimer laser photolysis of peroxodisulfate anions (S₂O ₈ ^2– ) at 351 nm followed by the reactions of sulfate radicals (SO ₄ ^– ) with excess nitrate. The time-resolved detection of NO₃ was achieved by long-path laser absorption at 632.8 nm. For the reactions of NO₃ with formic acid (1) and formate (2) rate coefficients ofk ₁=(3.3±1.0)×10⁵ l mol^–1 s^–1 andk ₂=(5.0±0.4)×10⁷ l mol^–1 s^–1 were found atT=298 K andI=0.19 mol/l. The following Arrhenius expressions were derived:k ₁(T)=(3.4±0.3)×10¹⁰ exp[–(3400±600)/T] l mol^–1 s^–1 andk ₂(T)=(8.2±0.8)×10¹⁰ exp[–(2200±700)/T] l mol^–1 s^–1. The rate coefficients for the reactions of NO₃ with acetic acid (3) and acetate (4) atT=298 K andI=0.19 mol/l were determined as:k ₃=(1.3±0.3)×10⁴ l mol^–1 s^–1 andk ₄=(2.3±0.4)×10⁶ l mol^–1 s^–1. The temperature dependences for these reactions are described by:k ₃(T)=(4.9±0.5)×10⁹ exp[–(3800±700)/T] l mol^–1 s^–1 andk ₄(T)=(1.0±0.2)×10¹² exp[–(3800±1200)/T] l mol^–1 s^–1. The differences in reactivity of the anions HCOO^– and CH₃COO^– compared to their corresponding acids HCOOH and CH₃COOH are explained by the higher reactivity of NO₃ in charge transfer processes compared to H atom abstraction. From a comparison of NO₃ reactions with various droplets constituents it is concluded that the reaction of NO₃ with HCOO^– may present a dominant loss reaction of NO₃ in atmospheric droplets.  相似文献   

Reservoir timescales for anthropogenic CO2 in the atmosphere     

O'Neill BC  Gaffin SR  Tubiello FN  Oppenheimer M 《Tellus. Series B, Chemical and physical meteorology》1994,46(5):378-389

Non-steady state timescales are complicated and their application to specific geophysical systems requires a common theoretical foundation. We first extend reservoir theory by quantifying the difference between turnover time and transit time (or residence time) for time-dependent systems under any mixing conditions. We explicitly demonstrate the errors which result from assuming these timescales are equal, which is only true at steady state. We also derive a new response function which allows the calculation of age distributions and timescales for well-mixed reservoirs away from steady state, and differentiate between timescales based on gross and net fluxes. These theoretical results are particularly important to tracer-calibrated "box models" currently used to study the carbon cycle, which usually approximate reservoirs as well-mixed. We then apply the results to the important case of anthropogenic CO2 in the atmosphere, since timescales describing its behavior are commonly used but ambiguously defined. All relevant timescales, including lifetime, transit time, and adjustment time, are precisely defined and calculated from data and models. Apparent discrepancies between the current, empirically determined turnover time of 30-60 years and longer model-derived estimates of expected lifetime and adjustment time are explained within this theoretical framework. We also discuss the results in light of policy issues related to global warming, in particular since any comparisons of the "lifetimes" of different greenhouse gases (CO2, CH4, N2O, CFC's etc.) must use a consistent definition to be meaningful.  相似文献