Competitive Exclusion of Sulfate Reduction by Fe(lll)-Reducing Bacteria: A Mechanism for Producing Discrete Zones of High-Iron Ground Water     

Francis H. Chapelle  Derek R. Lovley 《Ground water》1992,30(1):29-36

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New North Sea association     

Derek Ellis 《Marine pollution bulletin》1985,16(6):221-224

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Environmental Anarchy     

Derek Ellis 《Marine pollution bulletin》1985,16(7):259-260

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Relationships between marginal thrusting and movement on major,internal shear zones in the Northern Highland Caledonides,Scotland     

Simon P Kelley  Derek Powell 《Journal of Structural Geology》1985,7(2):161-174

The development of the syn-metamorphic Sgurr Beag slide zone, a major ductile shear zone of initially low dip, caused at least 50 km north-western thrust displacement of part of the internal metamorphic complex of the Northern Highland Caledonides of Scotland. Initiation of the zone, and movements upon it, were earlier than formation of the marginal Moine Thrust zone. Movement on the zone followed but overlapped the peak Caledonian metamorphism and the mid to high amphibolite facies mineral assemblages, fabrics and structures produced during the development of the slide zone and those surviving from earlier events, were reworked under greenschist facies conditions during mylonitization associated with initiation of the Moine Thrust zone. Displacements on the slide zone and thrust movements were separated by emplacement of a regional suite of pegmatites and a considerable change of metamorphic grade. Thus, they may not constitute members of a progressive sequence of Caledonian thrusts formed over a short time interval. Rather, preliminary isotopic data may imply an interval of c. 25 Ma between movement on the slide zone and final, ductile translation along the Moine Thrust zone.  相似文献   

A comparison of the reactions to government taxation measures of twentieth century mining companies and nineteenth century pastoralists     

Derek L Smith 《The Australian geographer》1995,26(1):61-70

This paper compares pastoralists in South Australia in the nineteenth century with Australian mining companies in the twentieth century as they resist the efforts of government to extract a greater proportion of the wealth created in the exploitation of natural resources. In effect, in both cases the struggle relates to the allocation of economic rent between private and corporate capital on the one hand, and the owners of the resources, the people of Australia, on the other. It is difficult not to be impressed by the similarities in the ideologies, objectives and strategies of these two groups of resource exploiters, separated though they are by over one hundred years.  相似文献   

Numerical simulations of granular dynamics II: Particle dynamics in a shaken granular material     

Naomi Murdoch  Patrick Michel  Derek C. Richardson  Kerstin Nordstrom  Christian R. Berardi  Simon F. Green  Wolfgang Losert 《Icarus》2012,219(1):321-335

Surfaces of planets and small bodies of our Solar System are often covered by a layer of granular material that can range from a fine regolith to a gravel-like structure of varying depths. Therefore, the dynamics of granular materials are involved in many events occurring during planetary and small-body evolution thus contributing to their geological properties.We demonstrate that the new adaptation of the parallel N-body hard-sphere code pkdgrav has the capability to model accurately the key features of the collective motion of bidisperse granular materials in a dense regime as a result of shaking. As a stringent test of the numerical code we investigate the complex collective ordering and motion of granular material by direct comparison with laboratory experiments. We demonstrate that, as experimentally observed, the scale of the collective motion increases with increasing small-particle additive concentration.We then extend our investigations to assess how self-gravity and external gravity affect collective motion. In our reduced-gravity simulations both the gravitational conditions and the frequency of the vibrations roughly match the conditions on asteroids subjected to seismic shaking, though real regolith is likely to be much more heterogeneous and less ordered than in our idealised simulations. We also show that collective motion can occur in a granular material under a wide range of inter-particle gravity conditions and in the absence of an external gravitational field. These investigations demonstrate the great interest of being able to simulate conditions that are to relevant planetary science yet unreachable by Earth-based laboratory experiments.  相似文献   

N-body simulations of cohesion in dense planetary rings: A study of cohesion parameters     

Randall P. Perrine  Derek C. Richardson 《Icarus》2012,219(2):515-533

We present results from a large suite of simulations of Saturn’s dense A and B rings using a new model of particle sticking in local simulations (Perrine, R.P., Richardson, D.C., Scheeres, D.J. [2011]. Icarus 212, 719–735). In this model, colliding particles can be incorporated into or help fragment rigid aggregations on the basis of certain user-specified parameters that can represent van der Waals forces or interlocking surface frost layers.Our investigation is motivated by laboratory results that show that interpenetration of surface layers can allow impacting frost-covered ice spheres to stick together. In these experiments, cohesion only occurs below specific impact speeds, which happen to be characteristic of impact speeds in Saturn’s rings. Our goal is to determine if weak bonding is consistent with ring observations, to constrain cohesion parameters in light of existing ring observations, to make predictions about particle populations throughout the rings, and to discover other diagnostics that may constrain bonding parameters.We considered the effects of five parameters on the equilibrium characteristics of our ring simulations: speed-based merge and fragmentation limits, bond strength, ring surface density, and patch orbital distance (i.e., the A or B ring), some with both monodisperse and polydisperse comparison cases. In total, we present data from 95 simulations.We find that weak cohesion is consistent with observations of the A and B rings (e.g., French, R.G., Nicholson, P.D. [2000]. Icarus 145, 502–523), and we present a range of simulation parameters that reproduce the observed size distribution and maximum particle size. It turns out that the parameters that match observations differ between the A and B rings, and we discuss the potential implications of this result. We also comment on other observable consequences of cohesion for the rings, such as optical depth and scale height effects, and discuss whether very large objects (e.g., “propeller” source objects) are grown bottom-up from cohesion of smaller ring particles.  相似文献   

A multiphysics and multiscale software environment for modeling astrophysical systems     

Simon Portegies Zwart  Steve McMillan  Stefan Harfst  Derek Groen  Michiko Fujii  Breanndán Ó Nualláin  Evert Glebbeek  Douglas Heggie  James Lombardi  Piet Hut  Vangelis Angelou  Sambaran Banerjee  Houria Belkus  Tassos Fragos  John Fregeau  Evghenii Gaburov  Rob Izzard  Mario Jurić  Stephen Justham  Andrea Sottoriva  Marcel Zemp 《New Astronomy》2009,14(4):369-378

We present MUSE, a software framework for combining existing computational tools for different astrophysical domains into a single multiphysics, multiscale application. MUSE facilitates the coupling of existing codes written in different languages by providing inter-language tools and by specifying an interface between each module and the framework that represents a balance between generality and computational efficiency. This approach allows scientists to use combinations of codes to solve highly coupled problems without the need to write new codes for other domains or significantly alter their existing codes. MUSE currently incorporates the domains of stellar dynamics, stellar evolution and stellar hydrodynamics for studying generalized stellar systems. We have now reached a “Noah’s Ark” milestone, with (at least) two available numerical solvers for each domain. MUSE can treat multiscale and multiphysics systems in which the time- and size-scales are well separated, like simulating the evolution of planetary systems, small stellar associations, dense stellar clusters, galaxies and galactic nuclei. In this paper we describe three examples calculated using MUSE: the merger of two galaxies, the merger of two evolving stars, and a hybrid N-body simulation. In addition, we demonstrate an implementation of MUSE on a distributed computer which may also include special-purpose hardware, such as GRAPEs or GPUs, to accelerate computations. The current MUSE code base is publicly available as open source at http://muse.li.  相似文献   

西天山东塔尔别克金矿区安山岩LA-ICP-MS锆石U-Pb年代学、元素地球化学与岩石成因   总被引：10，自引：7，他引：3  

唐功建  王强  赵振华  Derek A WYMAN  陈海红  贾小辉  姜子琦 《岩石学报》2009,25(6):1341-1352

东塔尔别克金矿区位于西天山吐拉苏盆地内阿希金矿区南侧,构造上属于伊犁-中天山微板块与准噶尔板块之间的博罗科努早古生代岛弧带西段。东塔尔别克矿区出露有一些安山岩,这些岩石具有典型高镁安山岩特征,如高硅（SiO₂=58.94%~63.85%),具有较高的MgO含量(3.75%~6.59%)和Mg^#(58~69)、高的Cr（94.2×10^-6~241×10^-6）、和Ni（54.5×10^-6~126 ×10^-6）含量,以及低的FeO^T/MgO比值。除了Sr含量略微偏低（235×10^-6~696×10^-6）之外,这些岩石基本显示了埃达克岩的地球化学特征：高的Al₂O₃（15.39%~16.65%）,低Y（9.86×10^-6~14.9×10^-6）含量,以及高的Sr/Y比值(23.8~48.1),无Eu异常,Nb、Ta、Ti亏损等。LA-ICP-MS锆石U-Pb测年结果显示安山岩的年龄为347.2±1.6Ma,为早石炭世。安山岩富集Rb、Th、U 等大离子亲石元素,相对亏损Nb、Ta、Ti等高场强元素,轻重稀土元素分馏明显,具有俯冲带岛弧岩浆的特征。东塔尔别克安山岩可能形成于岛弧环境中,并可能由俯冲的晚古生代北天山洋洋壳以及少量上覆沉积物熔融形成,产生的熔体在上升过程中与地幔橄榄岩发生了相互作用. 熔体-地幔相互作用对区内金矿的形成具有重要意义。  相似文献   

A possible glacially-forced tectonic mechanism for late Neogene surface uplift and subsidence around the North Atlantic     

Derek J. Blundell  David A. Waltham 《Proceedings of the Geologists' Association. Geologists' Association》2009,120(2-3):98-107

Analysis of old erosion surfaces and estimates of exhumation from apatite fission track data can be used to infer late Neogene surface uplift of Britain, Greenland, Norway and Svalbard of 1–2 km. Subsidence and sedimentation in adjacent offshore basins can be found from interpretation of seismic and well log data. Various mechanisms for surface uplift have been proposed but the underlying cause remains unexplained. Since the multiple glaciations that took place during the late Neogene were a common factor, a possible glacially-forced tectonic mechanism to thicken the crust and produce surface uplift has been investigated. This could result from the relatively slow accumulation of ice that loads the crust as an ice sheet grows during a glacial period, followed by relatively rapid retreat and unloading around its periphery at the end. Unloading could create transient stresses that induce lateral flow in a ductile lower crust to thicken it onshore and produce surface uplift, with associated thinning beneath adjacent offshore basins, producing subsidence. Simple calculations show that the proposed mechanism is feasible and indicate that crustal thickening and surface uplift accumulated from a number of glacial cycles can account for the observed surface uplift, with an acceptable flow rate in the lower crust at the end of each cycle if the viscosity of ductile flow is sufficiently low.  相似文献