In situ bioremediation of trichloroethylene-contaminated water by a resting-cell methanotrophic microbial filter     

R. T. TAYLOR  M. L. HANNA  N. N. SHAH  D. R. SHONNARD  A. G. DUBA  W. B. DURHAM 《水文科学杂志》2013,58(4):323-342

Abstract

An in situ microbial filter technology is being tested and developed for remediating migrating subsurface plumes contaminated with low concentrations of trichloroethylene (TCE). The current focus is the establishment of a replenishable bioactive zone (catalytic filter) along expanding plume boundaries by the injection of a representative methanotrophic bacterium, Methylosinus trichosporium OB3b. This microbial filter strategy has been successfully demonstrated using emplaced, attached resting cells (no methane additions) in a 1.1 m flow-through test bed loaded with water-saturated sand. Two separate 24 h pulses of TCE (109 ppb and 85 ppb), one week apart, were pumped through the system at a flow velocity of 15 mm h^?1; no TCE (< 0.5 ppb) was detected on the downstream side of the microbial filter. Subsequent excavation of the wet sand confirmed the existence of a TCE-bioactive zone 21 days after it had been created. An enhanced longevity of the cellular, soluble-form methane monooxygenase produced by this methanotroph is a result of the laboratory bioreactor culturing conditions. Additional experiments with cells in sealed vials and emplaced in the 1.1 m test bed yielded a high resting-cell finite TCE biotransformation capacity of about 0.25 mg per mg of bacteria; this is suitable for a planned sand-filled trench field demonstration at a Lawrence Livermore National Laboratory site.  相似文献   

Fossils explained 6: Bryozoans     

PAUL D. TAYLOR 《Geology Today》1986,2(5):152-153

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西秦岭温泉钼矿床成矿作用时限及其对斑岩型钼矿床系统分类制约   总被引：6，自引：4，他引：2  

邱昆峰  李楠  RyanDTAYLOR  宋耀辉  宋开瑞  韩旺珍  张东旭 《岩石学报》2014,30(9):2631-2643

斑岩系统是一个涉及岩浆和热液作用的复杂系统,建立精细的斑岩系统成因模型对于寻找更为丰富的金属矿产尤为重要,成矿作用时限是建立成因模型和指导矿产勘查的关键。温泉钼矿床是西秦岭造山带内与晚三叠世花岗岩有关的斑岩型钼矿床,其在西秦岭造山带的独特发育蕴含印支期斑岩成矿作用、大陆地壳演化及矿产勘查关键科学问题。钼矿体主要赋存于温泉复式岩体Ⅱ单元和Ⅲ单元的黑云母二长花岗斑岩和似斑状二长花岗岩中,钼以细脉和浸染状矿化形式产出。赋矿岩石单元锆石U-Pb年龄为224.6±2.5Ma到216.2±1.7Ma,Ⅱ和Ⅲ单元分别侵位于~223Ma和~217Ma,持续约8Myr。辉钼矿Re-Os年龄为212.7±2.6Ma到215.1±2.6Ma,暗示晚三叠世钼成矿作用与花岗质岩浆作用密切时空关系,且成矿年龄稍晚,反映钼矿化主要发生在岩浆作用晚期阶段。成岩、成矿作用发生于华北板块与华南板块全面对接后秦岭造山带构造体制由碰撞到后碰撞的转折阶段,响应南秦岭变质变形、勉-略洋盆闭合及大别-苏鲁超高压岩石板片折返统一地质事件。黑云母K-Ar年龄为207~226Ma,可能反映~223Ma和~208Ma的岩体冷却事件和~216Ma的岩浆-热液成矿作用。锆石U-Pb、辉钼矿Re-Os和黑云母K-Ar多元同位素定年系统准确刻画岩体侵位、热液成矿与冷却事件上有所重叠,岩浆-热液分异演化充分,且具有较高的冷却速率,精确厘定温泉斑岩系统岩浆活动的"多期性"(复式岩体)、成矿事件的"瞬时性"(~214Ma)和成矿作用的"持续性"(~8Myr)。同时,系统对比全球典型斑岩钼(铜)矿床成矿动力学背景,细化分类方案,即产于挤压背景的大洋俯冲和大陆碰撞环境矿床及产于伸展背景的后碰撞、陆缘弧后和板内裂谷环境矿床。明确在大洋俯冲→大陆碰撞→后碰撞→板内裂谷旋回的四个阶段均可以产生规模的斑岩型钼(铜)矿床,且挤压向伸展过渡的构造体制转换尤其是大型矿床形成的有利环境。  相似文献   

Preparing For Hyperseed MAC: An Observing Campaign To Monitor The Entry Of The Genesis Sample Return Capsule     

PETER JENNISKENS  PAUL WERCINSKI  JOE OLEJNICZAK  GARY ALLEN  PRASUN N. DESAI  GEORGE RAICHE  DEAN KONTINOS  DOUG REVELLE  JASON HATTON  RICHARD L. BAKER  RAY W. RUSSELL  MIKE TAYLOR  FRANS RIETMEIJER 《Earth, Moon, and Planets》2004,95(1-4):339-360

The imminent return of the Genesis Sample Return Capsule (SRC) from the Earth’s L1 point on September 8, 2004, represents the first opportunity since the Apollo era to study the atmospheric entry of a meter-sized body at or above the Earth’s escape speed. Until now, reentry heating models are based on only one successful reentry with an instrumented vehicle at higher than escape speed, the 22 May 1965 NASA “FIRE 2” experiment. In preparation of an instrumented airborne and ground-based observing campaign, we examined the expected bolide radiation for the reentry of the Genesis SRC. We find that the expected emission spectrum consists mostly of blackbody emission from the SRC surface (T∼ ∼2630 K@peak heating), slightly skewed in shape because of a range of surface temperatures. At high enough spectral resolution, shock emission from nitrogen and oxygen atoms, as well as the first positive and first negative bands of N₂⁺, will stand out above this continuum. Carbon atom lines and the 389-nm CN band emission may also be detected, as well as the mid-IR 4.6-μm CO band. The ablation rate can be studied from the signature of trace sodium in the heat shield material, calibrated by the total amount of matter lost from the recovered shield. A pristine collection of the heat shield would also permit the sampling of products of ablation.  相似文献   

Melt Generation and Fluid Flow in the Thermal Aureole of the Bushveld Complex   总被引：2，自引：0，他引：2  

HARRIS  NIGEL; McMILLAN  ANDY; HOLNESS  MARIAN; UKEN  RON; WATKEYS  MIKE; ROGERS  NICK; FALLICK  ANTHONY 《Journal of Petrology》2003,44(6):1031-1054

Granite sheets emplaced into the migmatite zone of the easterncontact aureole of the Bushveld Complex resulted from fluid-enhanced,incongruent biotite melting of the underlying Silverton Formationshales during prograde metamorphism. Ba concentrations are extremein both the sheets (>1000 ppm) and the hornfels (>800ppm) into which they have been emplaced. We conclude that aBa-rich, hydrothermal fluid induced melting in the aureole,and that fluid transport of Ba²⁺, and to a lesser extent, Sr²⁺and Eu²⁺, persisted in the melt zones under subsolidus conditions.Sr-isotope systematics from high-Ba localities define an errorchronof 2161 ± 106 Ma with an initial (⁸⁷Sr/⁸⁶Sr) ratio of0·705 ± 0·001. Metasedimentary rocks unaffectedby fluid infiltration were homogenized at the same time butwith an increased initial ratio, suggesting that whereas isotopehomogenization was achieved between outcrops permeated by fluids,there is no evidence of regional homogenization. Oxygen-isotopecompositions of psammitic metasediments in the aureole are uncorrelatedwith distance from the contact, suggesting the infiltratingfluid equilibrated isotopically with the metasediments. Theirelevated  相似文献   

The Leonard Award Address Presented 1998 July 27, Dublin,Ireland: On the difficulties of making Earth-like planets     

Stuart Ross TAYLOR 《Meteoritics & planetary science》1999,34(3):317-329

Abstract— Here I discuss the series of events that led to the formation and evolution of our planet to examine why the Earth is unique in the solar system. A multitude of factors are involved: These begin with the initial size and angular momentum of the fragment that separated from a molecular cloud; such random factors are crucial in determining whether a planetary system or a double star develops from the resulting nebula. Another requirement is that there must be an adequate concentration of heavy elements to provide the 2% “rock” and “ice” components of the original nebula. An essential step in forming rocky planets in the inner nebula is the loss of gas and depletion of volatile elements, due to early solar activity that is linked to the mass of the central star. The lifetime of the gaseous nebula controls the formation of gas giants. In our system, fine timing was needed to form the gas giant, Jupiter, before the gas in the nebula was depleted. Although Uranus and Neptune eventually formed cores large enough to capture gas, they missed out and ended as ice giants. The early formation of Jupiter is responsible for the existence of the asteroid belt (and our supply of meteorites) and the small size of Mars, whereas the gas giant now acts as a gravitational shield for the terrestrial planets. The Earth and the other inner planets accreted long after the giant planets, from volatile-depleted planetesimals that were probably already differentiated into metallic cores and silicate mantles in a gas-free, inner nebula. The accumulation of the Earth from such planetesimals was essentially a stochastic process, accounting for the differences among the four rocky inner planets—including the startling contrast between those two apparent twins, Earth and Venus. Impact history and accretion of a few more or less planetesimals were apparently crucial. The origin of the Moon by a single massive impact with a body larger than Mars accounts for the obliquity (and its stability) and spin of the Earth, in addition to explaining the angular momentum, orbital characteristics, and unique composition of the Moon. Plate tectonics (unique among the terrestrial planets) led to the development of the continental crust on the Earth, an essential platform for the evolution of Homo sapiens. Random major impacts have punctuated the geological record, accentuating the directionless course of evolution. Thus a massive asteroidal impact terminated the Cretaceous Period, resulted in the extinction of at least 70% of species living at that time, and led to the rise of mammals. This sequence of events that resulted in the formation and evolution of our planet were thus unique within our system. The individual nature of the eight planets is repeated among the 60-odd satellites—no two appear identical. This survey of our solar system raises the question whether the random sequence of events that led to the formation of the Earth are likely to be repeated in detail elsewhere. Preliminary evidence from the “new planets” is not reassuring. The discovery of other planetary systems has removed the previous belief that they would consist of a central star surrounded by an inner zone of rocky planets and an outer zone of giant planets beyond a few astronomical units (AU). Jupiter-sized bodies in close orbits around other stars probably formed in a similar manner to our giant planets at several astronomical units from their parent star and, subsequently, migrated inwards becoming stranded in close but stable orbits as “hot Jupiters”, when the nebula gas was depleted. Such events would prevent the formation of terrestrial-type planets in such systems.  相似文献   

Formation of a martian pyroxenite: A comparative study of the nakhlite meteorites and Theo's Flow     

R. C. FRIEDMAN LENTZ  G. J. TAYLOR  A. H. TREIMAN 《Meteoritics & planetary science》1999,34(6):919-932

Abstract— The unusual composition of the nakhlites, a group of pyroxenitic martian meteorites with young ages, presents an opportunity to learn about nonbasaltic magmatic activity on another planet. However, the limited number of these meteorites makes unraveling their history difficult. A promising terrestrial analog for the formation of the nakhlites is Theo's Flow in Ontario, Canada. This atypical, 120 m-thick flow differentiated in place, forming distinct layered lithologies of peridotite, pyroxenite, and gabbro. Theo's pyroxenite and the nakhlites share strikingly similar petrographies, with concentrated euhedral to subhedral augite grains set in a plagioclase-rich matrix. These two suites of rocks also share specific petrologic features, mineral and whole-rock compositional features, and size and spatial distributions of cumulus grains. The numerous similarities suggest that the nakhlites formed by a similar mechanism in a surface lava flow or shallow intrusion. Their formation could have involved settling of crystals in a phenocryst-laden flow or in situ nucleation and growth of pyroxenes in an ultramafic lava flow. The latter case is more likely and requires steady-state nucleation and growth of clusters of pyroxene grains (and olivine in the nakhlites), circulating in a strongly convecting melt pool, followed by settling and continued growth in a thickening cumulate pile. Trapped pockets of intercumulus liquid in the pile gradually evolved, finally growing Fe-enriched rims on cumulus grains. With sufficient evolution, the melt reached plagioclase supersaturation, causing rapid growth of plagioclase sprays and late-stage mesostasis growth.  相似文献   

Martian basalt (shergottite) Queen Alexandra Range 94201 and lunar basalt 15555: A tale of two pyroxenes     

M. WADHWA  G. CROZAZ  L. A. TAYLOR  H. Y. MCSWEEN 《Meteoritics & planetary science》1998,33(2):321-328

Abstract— We present here ion microprobe analyses of rare earth and other selected trace and minor elements in pyroxenes of shergottite Queen Alexandra Range 94201 and lunar basalt 15555. Pyroxene zonation patterns record the crystallization histories of these two basaltic samples from Mars and the Moon, respectively, and allow a comparison of mafic melt evolution on these two planetary bodies. Elemental abundances and trends in pyroxenes of these two rocks indicate that their minerals formed by continuous, closed system fractional crystallization of their respective parent melts. This further supports the idea that QUE 94201 closely represents the composition of a true Martian basaltic melt (McSween et al., 1996). The main differences in pyroxene elemental zonation patterns in these two objects are attributed to earlier crystallization of whitlockite in QUE 94201 (i.e., before the Fe-rich pyroxenes) than in 15555 (after the Fe-rich pyroxenes). The size of Eu anomalies in pyroxenes of QUE 94201 is intermediate between that in pyroxenes of 15555 and the other shergottites and may imply that fO₂ conditions during crystallization of this Martian basalt were significantly more reducing than for other shergottites, although not quite as reducing as for lunar basalts. Cerium anomalies appear to be less prevalent in pyroxenes of QUE 94201 than other Antarctic shergottites and could be indicative of lesser degree of weathering in the Antarctic.  相似文献   

Spatial Monopoly and Functional Economic Regions: The Impact of Manufacturers' Limited Spatial Knowledge in the New Zealand Space Economy     

M.J. TAYLOR  P.L. HOSKING 《New Zealand geographer》1979,35(1):3-15

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The Lyme Regis borehole of 1901: a lesson for everyone     

MICHAEL A. TAYLOR 《Geology Today》1989,5(6):209-211

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