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  • Conference paper
    Almeida T, Muxworthy AR, Williams W, 2013,

    Magnetic characterization of synthetic titanomagnetites

    , IAGA
  • Conference paper
    Almeida T, Muxworthy AR, Wiliams W, Dunin-Borkowski Ret al., 2013,

    Oxidation of pseudo-single domain Fe3O4 particles and associated magnetic response examined by environmental TEM and off-axis electron holography

    , Microscopy and Microanalysis 2013 Annual Meeting
  • Journal article
    Emmerton S, Muxworthy AR, Sephton MA, Aldana M, Costanzo-Alvarez V, Bayona G, Williams Wet al., 2013,

    Correlating biodegradation to magnetization in oil bearing sedimentary rocks

    , GEOCHIMICA ET COSMOCHIMICA ACTA, Vol: 112, Pages: 146-165, ISSN: 0016-7037
  • Conference paper
    Genge MJ, 2013,


    , 76th Annual Meeting of the Meteoritical-Society, Publisher: WILEY-BLACKWELL, Pages: A141-A141, ISSN: 1086-9379
  • Conference paper
    Bland PA, Collins GS, Dyl KA, Abreu NM, Davison TM, Ciesla FJ, Muxworthy AR, Moore Jet al., 2013,

    Impact-induced compaction of primordial materials and the effect on the chondrite record.

    , 76th Annual Meeting of the Meteoritical-Society, Publisher: WILEY-BLACKWELL, Pages: A63-A63, ISSN: 1086-9379
  • Conference paper
    Almeida T, Muxworthy AR, Williams W, Dunin-Borkowski Ret al., 2013,

    Complementary electron energy loss spectroscopy and off-axis electron holography investigation of the chemical remanent magnetisation of synthetic magnetic recorders

    , Electron Microscopy and Analysis Group Conference
  • Conference paper
    Van Ginneken M, Muxworthy A, Genge M, 2013,

    First-Order Reversal Curves (FORC) analysis of micrometeorites

    , 76th Annual Meteoritical Society Meeting
  • Journal article
    Oishi Y, Piggott MD, Maeda T, Kramer SC, Collins GS, Tsushima H, Furumura Tet al., 2013,

    Three-dimensional tsunami propagation simulations using an unstructured mesh finite element model

    , Journal of Geophysical Research: Solid Earth, Vol: 118, Pages: 2998-3018, ISSN: 2169-9313
  • Journal article
    Carter JN, Sephton MA, 2013,

    A Bayesian statistical assessment of representative samples for asteroidal or meteoritical material

    , Meteoritics & Planetary Science, Vol: 48, Pages: 976-996, ISSN: 1086-9379
  • Journal article
    Muxworthy AR, Evans ME, Scourfield S, King JGet al., 2013,

    Paleointensity results from the late-Archaean Modipe gabbro of Botswana

    , Geochemistry Geophysics Geosystems
  • Journal article
    Sephton MA, 2013,

    Aromatic units from the macromolecular material in meteorites: Molecular probes of cosmic environments

    , Geochimica et Cosmochimica Acta, Vol: 107, Pages: 231-241, ISSN: 0016-7037
  • Conference paper
    Abubakar R, Muxworthy AR, Sephton MA, Fraser Aet al., 2013,

    Experimental investigation of magnetic mineral formation in hydrocarbon environments

    , EGU
  • Journal article
    Lappe S-CLL, Feinberg J, Muxworthy A R, Harrison Ret al., 2013,

    Comparison and calibration of non-heating paleointensity methods: A case study using dusty olivine

    , Geochemistry Geophysics Geosystems
  • Journal article
    Muxworthy AR, 2013,

    The role of magnetic interactions in natural systems

    , Astronomy & Geophysics, Vol: 54, Pages: 31-35
  • Journal article
    Biggin AJ, Badejo S, Hodgson E, Muxworthy AR, Shaw J, Dekkers MJet al., 2013,

    The effect of cooling rate on the intensity of thermoremanent magnetization (TRM) acquired by assemblages of pseudo-single domain, multidomain and interacting single-domain grains

    , Geophysical Journal International
  • Journal article
    Abouchami W, Galer SJG, Horner TJ, Rehkaemper M, Wombacher F, Xue Z, Lambelet M, Gault-Ringold M, Stirling CH, Schoenbaechler M, Shiel AE, Weis D, Holdship PFet al., 2013,

    A Common Reference Material for Cadmium Isotope Studies - NIST SRM 3108

    , GEOSTANDARDS AND GEOANALYTICAL RESEARCH, Vol: 37, Pages: 5-17, ISSN: 1639-4488
  • Journal article
    Voldman GG, Genge MJ, Albanesi GL, Barnes CR, Ortega Get al., 2013,

    Cosmic spherules from the Ordovician of Argentina

    , GEOLOGICAL JOURNAL, Vol: 48, Pages: 222-235, ISSN: 0072-1050
  • Journal article
    Warner M, Ratcliffe A, Nangoo T, Morgan J, Umpleby A, Shah N, Vinje V, Stekl I, Guasch L, Win C, Conroy G, Bertrand Aet al., 2013,

    Anisotropic 3D full-waveform inversion

    , Geophysics, Vol: 78, Pages: R59-R80

    We have developed and implemented a robust and practical scheme for anisotropic 3D acoustic full-waveform inversion (FWI). We demonstrate this scheme on a field data set, applying it to a 4C ocean-bottom survey over the Tommeliten Alpha field in the North Sea. This shallow-water data set provides good azimuthal coverage to offsets of 7 km, with reduced coverage to a maximum offset of about 11 km. The reservoir lies at the crest of a high-velocity antiformal chalk section, overlain by about 3000 m of clastics within which a low-velocity gas cloud produces a seismic obscured area. We inverted only the hydrophone data, and we retained free-surface multiples and ghosts within the field data. We invert in six narrow frequency bands, in the range 3 to 6.5 Hz. At each iteration, we selected only a subset of sources, using a different subset at each iteration; this strategy is more efficient than inverting all the data every iteration. Our starting velocity model was obtained using standard PSDM model building including anisotropic reflection tomography, and contained epsilon values as high as 20%. The final FWI velocity model shows a network of shallow high-velocity channels that match similar features in the reflection data. Deeper in the section, the FWI velocity model reveals a sharper and more-intense low-velocity region associated with the gas cloud in which low-velocity fingers match the location of gas-filled faults visible in the reflection data. The resulting velocity model provides a better match to well logs, and better flattens common-image gathers, than does the starting model. Reverse-time migration, using the FWI velocity model, provides significant uplift to the migrated image, simplifying the planform of the reservoir section at depth. The workflows, inversion strategy, and algorithms that we have used have broad application to invert a wide-range of analogous data sets.

  • Journal article
    Gulick S, Christeson G, Barton P, Grieve R, Morgan J, Urrutia Jet al., 2013,

    Geophysical Characterization of the Chicxulub Impact Crater

    , Reviews of Geophysics

    Geophysical data indicate that the 65.5 Ma Chicxulub impact structure is a multi-ring basin, with three sets of semi-continuous, arcuate ring faults and a topographic peak ring. Slump blocks define a terrace zone, which steps down from the inner rim into the annular trough. Fault blocks underlie the peak ring, which exhibits variable relief, due to target asymmetries. The central structural uplift is >10 km and the Moho is displaced by 1-2 km. The working hypothesis for the formation of Chicxulub is: a 50 km radius transient cavity, lined with melt and impact breccia, formed within 10s of seconds of the impact and within minutes, weakened rebounding crust rose kilometers above the surface, the transient crater rim underwent localized deformation and collapsed into large slump blocks, resulting in a inner rim at 70-85 km radius, and outer ring faults at 70-130 km radius. The over-heightened structural uplift collapsed outwards, buried the inner slump blocks, and formed the peak ring. Most of the impact melt was ultimately emplaced as a coherent <3-km thick melt sheet within the central basin that shallows within the inner regions of the peak ring. Smaller pockets of melt flowed into the annular trough. Subsequently, slope collapse, ejecta, ground surge, and tsunami waves infilled the annular trough and annular basin with sediments up to 3 km and 900 m thick, respectively. Testing this working hypothesis requires direct observation of the impactites, within and adjacent to the peak ring and central basin.

  • Journal article
    Miljković K, Collins GS, Mannick S, Bland PAet al., 2013,

    Morphology and population of binary asteroid impact craters

    , Earth and Planetary Science Letters, Vol: 363, Pages: 121-132, ISSN: 0012-821X

    Observational data show that in the Near Earth Asteroid (NEA) region 15% of asteroids are binary. However, the observed number of plausible doublet craters is 2–4% on Earth and 2–3% on Mars. This discrepancy between the percentage of binary asteroids and doublets on Earth and Mars may imply that not all binary systems form a clearly distinguishable doublet crater owing to insufficient separation between the binary components at the point of impact. We simulate the crater morphology formed in close binary asteroid impacts in a planetary environment and the range of possible crater morphologies includes: single (circular or elliptical) craters, overlapping (tear-drop or peanut shaped) craters, as well as clearly distinct, doublet craters. While the majority of binary asteroids impacting Earth or Mars should form a single, circular crater, about one in four are expected to form elongated or overlapping impact craters and one in six are expected to be doublets. This implies that doublets are formed in approximately 2% of all asteroid impacts on Earth and that elongated or overlapping binary impact craters are under-represented in the terrestrial crater record. The classification of a complete range of binary asteroid impact crater structures provides a template for binary asteroid impact crater morphologies, which can help in identifying planetary surface features observed by remote sensing.

This data is extracted from the Web of Science and reproduced under a licence from Thomson Reuters. You may not copy or re-distribute this data in whole or in part without the written consent of the Science business of Thomson Reuters.

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