A new ‘microstructural mapping’ methodology for the identification,analysis and interpretation of polyphase deformation within subglacial sediments     

Emrys Phillips  Jaap J.M. van der Meer  Amanda Ferguson 《Quaternary Science Reviews》2011,30(19-20):2570-2596

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Comparison of central pit craters on Mars,Mercury, Ganymede,and the Saturnian satellites          下载免费PDF全文

Nadine G. Barlow  Sierra N. Ferguson  Ryan M. Horstman  Aviva Maine 《Meteoritics & planetary science》2017,52(7):1371-1387

We report on the first results of a large‐scale comparison study of central pit craters throughout the solar system, focused on Mars, Mercury, Ganymede, Rhea, Dione, and Tethys. We have identified 10 more central pit craters on Rhea, Dione, and Tethys than have previously been reported. We see a general trend that the median ratio of the pit to crater diameter (D_p/D_c) decreases with increasing gravity and decreasing volatile content of the crust. Floor pits are more common on volatile‐rich bodies while summit pits become more common as crustal volatile content decreases. Uplifted bedrock from below the crater floor occurs in the central peak upon which summit pits are found and in rims around floor pits, which may or may not break the surface. Peaks on which summit pits are found on Mars and Mercury share similar characteristics to those of nonpitted central peaks, indicating that some normal central peaks undergo an additional process to create summit pits. Martian floor pits do not appear to be the result of a central peak collapse as the median ratio of the peak to crater diameter (D_pk/D_c) is about twice as high for central peaks/summit pits than D_p/D_c values for floor pits. Median D_pk/D_c is twice as high for Mars as for Mercury, reflecting differing crustal strength between the two bodies. Results indicate that a complicated interplay of crustal volatiles, target strength, surface gravity, and impactor energy along with both uplift and collapse are involved in central pit formation. Multiple formation models may be required to explain the range of central pits seen throughout the solar system.  相似文献   

Gas/solid carbon branching ratios in surface‐mediated reactions and the incorporation of carbonaceous material into planetesimals          下载免费PDF全文

Joseph A. Nuth  Natasha M. Johnson  Frank T. Ferguson  Alicia Carayon 《Meteoritics & planetary science》2016,51(7):1310-1322

We report the ratio of the initial carbon available as CO that forms gas‐phase compounds compared to the fraction that deposits as a carbonaceous solid (the gas/solid branching ratio) as a function of time and temperature for iron, magnetite, and amorphous iron silicate smoke catalysts during surface‐mediated reactions in an excess of hydrogen and in the presence of N₂. This fraction varies from more than 99% for an amorphous iron silicate smoke at 673 K to less than 40% for a magnetite catalyst at 873 K. The CO not converted into solids primarily forms methane, ethane, water, and CO₂, as well as a very wide range of organic molecules at very low concentration. Carbon deposits do not form continuous coatings on the catalytic surfaces, but instead form extremely high surface area per unit volume “filamentous” structures. While these structures will likely form more slowly but over much longer times in protostellar nebulae than in our experiments due to the much lower partial pressure of CO, such fluffy coatings on the surfaces of chondrules or calcium aluminum inclusions could promote grain–grain sticking during low‐velocity collisions.  相似文献   

Research Note: Overpressure prediction from C‐wave seismic data     

Robert J. Ferguson  Daniel A. Ebrom  Kimberly M. Kumar 《Geophysical Prospecting》2011,59(4):787-792

Recently, mode converted shear waves (C‐waves) have been shown to enable overpressure prediction in media where primary wave acquisition is inhibited by gas and fluid effects – C‐wave moveout is analysed and a long standing relationship between differential stress and primary‐wave (P‐wave) velocity is modified and employed. Though pore‐pressure prediction based on C‐waves is supported by empirical evidence from laboratory and field experiments, a theoretical justification has yet to be developed. In this research note, we provide a supporting algebra for the original relationship between pore pressure and C‐wave velocity.  相似文献   

Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31     

R. Ibata  S. Chapman  A. M. N. Ferguson  M. Irwin  G. Lewis  A. McConnachie 《Monthly notices of the Royal Astronomical Society》2004,351(1):117-124

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The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?     

Blair C. Conn  Geraint F. Lewis  Mike J. Irwin  Rodrigo A. Ibata  Annette M. N. Ferguson  Nial Tanvir  Jonathan M. Irwin 《Monthly notices of the Royal Astronomical Society》2005,362(2):475-488

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The three-dimensional structure of the giant stellar stream in Andromeda   总被引：1，自引：0，他引：1  

A. W. McConnachie  M. J. Irwin  R. A. Ibata  A. M. N. Ferguson  G. F. Lewis  N. Tanvir 《Monthly notices of the Royal Astronomical Society》2003,343(4):1335-1340

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Textural evolution of perovskite in the Afrikanda alkaline–ultramafic complex,Kola Peninsula,Russia     

Naomi?J.?PotterEmail author  Matthew?R.?M.?Ferguson  Vadim?S.?Kamenetsky  Anton?R.?Chakhmouradian  Victor?V.?Sharygin  Jay?M.?Thompson  Karsten?Goemann 《Contributions to Mineralogy and Petrology》2018,173(12):100

Perovskite is a common accessory mineral in a variety of mafic and ultramafic rocks, but perovskite deposits are rare and studies of perovskite ore deposits are correspondingly scarce. Perovskite is a key rock-forming mineral and reaches exceptionally high concentrations in olivinites, diverse clinopyroxenites and silicocarbonatites in the Afrikanda alkaline–ultramafic complex (Kola Peninsula, NW Russia). Across these lithologies, we classify perovskite into three types (T1–T3) based on crystal morphology, inclusion abundance, composition, and zonation. Perovskite in olivinites and some clinopyroxenites is represented by fine-grained, equigranular, monomineralic clusters and networks (T1). In contrast, perovskite in other clinopyroxenites and some silicocarbonatites has fine- to coarse-grained interlocked (T2) and massive (T3) textures. Electron backscatter diffraction reveals that some T1 and T2 perovskite grains in the olivinites and clinopyroxenites are composed of multiple subgrains and may represent stages of crystal rotation, coalescence and amalgamation. We propose that in the olivinites and clinopyroxenites, these processes result in the transformation of clusters and networks of fine-grained perovskite crystals (T1) to mosaics of more coarse-grained (T2) and massive perovskite (T3). This interpretation suggests that sub-solidus processes can lead to the development of coarse-grained and massive perovskite. A combination of characteristic features identified in the Afrikanda perovskite (equigranular crystal mosaics, interlocked irregular-shaped grains, and massive zones) is observed in other oxide ore deposits, particularly in layered intrusions of chromitites and intrusion-hosted magnetite deposits and suggests that the same amalgamation processes may be responsible for some of the coarse-grained and massive textures observed in oxide deposits worldwide.  相似文献   

Some notes on radiation and long‐term climatic variations     

H. L. Ferguson 《大气与海洋》2013,51(4):133-152

Canadian definitions of break‐up and freeze‐up are shown to have changed substantially on several occasions since 1957. This paper demonstrates that because of these changes, great care must be exercised in the tabulation and interpretation of dates of break‐up and freeze‐up. In part, these changes have been occasioned by historical concerns, so that scrupulous attention to definition is necessary if the Canadian record is to be used for scientific purposes.  相似文献   

Redbed‐associated sabkhas and tidal flats at Shark Bay,Western Australia: Their significance for genetic models of stratiform Cu‐(Pb‐Zn) deposits     

J. Ferguson  G. W. Skyring 《Australian Journal of Earth Sciences》2013,60(4):321-333

Interaction of metalliferous continental brines with biogenic sulphide is the basis of some syngenetic and early diagenetic models for the formation of Cu‐(Pb‐Zn) sulphides during a depositional cycle of carbonates in restricted marine environments. A variation of these models (an ‘evaporative concentration‐lateral groundwater flow’ model) is proposed, using hydrological, geochemical and biological data from low metal, but otherwise pertinent redbed‐associated, sabkha, tidal flat and subtidal environments at Nilemah Embayment, in Hamelin Pool (Shark Bay, Western Australia).

The model is constrained by: (i) the short time available for ore accumulation during a single depositional cycle; (ii) limitation of adequate rates of bacterial sulphate reduction for the formation of an ore deposit to near‐surface sediments; (iii) restriction of the most favourable ore‐forming sites to the intertidal zone and the littoral shelf; (iv) coincidence in these sites of laterally‐flowing marine/meteoric groundwater brine, and mosaics of in situ cyanobacterial mats and shallow erosional depressions containing detrital organic matter eroded from the mats. Under these conditions the metalliferous fluid would have to contain about 1000 ppm Cu and flow for 1000 years at a rate of 5 m/a through the intertidal/littoral shelf environment to produce an ore deposit.

Critical features of a model that could generate this combination of very high metal concentrations and flow rates are: (i) a highly permeable unconfined aquifer system comprising alluvial fans at the base of basaltic mountain ranges and continental redbeds beneath a broad coastal plain; (ii) mobilization, concentration and transport of the metals in this aquifer to intertidal/littoral shelf sites of ore deposition; (iii) effective concentration processes in the aquifer, involving evaporation and reflux of brines in groundwater discharge areas on the coastal plain and evaporation in marine‐continental and marine sabkhas bordering the sites of deposition; (iv) rapid lateral groundwater flow of the concentrated metalliferous brines under a strong seawards‐directed hydraulic gradient; and (v) discharge of the metalliferous brines into or through topographic depressions generated by erosion and shoaling in the peritidal and littoral shelf environments.

The model hydrodynamic processes and their magnitude are within the range observed in modern environments but they are most likely to be effective in coarse‐grained, topographically irregular carbonate sabkhas and tidal flats, which usually form under high‐energy conditions. Even under these conditions, the individual ore‐forming processes must combine in an optimum manner before the highly demanding metal concentrations and flow rates required for ore formation in a single marine depositional cycle can be met.  相似文献