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1.
Gert Lube Shane J. Cronin Thomas Platz Armin Freundt Jonathan N. Procter Cargill Henderson Michael F. Sheridan 《Journal of Volcanology and Geothermal Research》2007
Small-volume pyroclastic density currents (PDCs) are generated frequently during explosive eruptions with little warning. Assessing their hazard requires a physical understanding of their transport and sedimentation processes which is best achieved by the testing of experimental and numerical models of geophysical mass flows against natural flows and/or deposits. To this end we report on one of the most detailed sedimentological studies ever carried out on a series of pristine small-volume PDC deposits from the 1975 eruption of Ngauruhoe volcano, whose emplacement were also witnessed during eruption. Using high-resolution GPS surveys, a series of lateral excavations across the deposits, and bulk sedimentological analysis we constrained the geomorphology, internal structure and texture of the deposits with respect to laterally varying modes of deposition. 相似文献
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Robert L. Brathwaite Hugh J. Cargill Anthony B. Christie Andrew Swain 《Mineralium Deposita》2001,36(1):1-12
Vein distributions in line samples from four epithermal Au–Ag deposits of the Hauraki Goldfield were logged and quantified
by vein spacing, vein density, vein thickness and percentage of vein extension. One deposit is hosted in andesite lavas (Martha
Hill), one in andesite lavas and dacite porphyry, dacitic tuffs and pyroclastic breccias (Golden Cross), and two in rhyolite
lavas and rhyolitic tuffs with minor andesite lavas or andesite dikes (Ohui and Wharekirauponga). The vein systems in these
deposits form fault-controlled arrays of extensional veins. Vein spacing distributions are non-fractal over two to three orders
of magnitude (1 mm to 5 m), and therefore fractal dimension statistics are not applicable. The coefficient of variation (Cv) of vein spacing was used as a measure of the degree of vein clustering. Rock type has a marked influence on vein spacing
distributions, with veining in rhyolite lava having lower average thickness and percentage extension, but a generally higher
degree of vein clustering compared with veining in andesite lava in the same deposit. Vein spacing distributions in well-jointed
lithologies, mainly andesite lava, have Cv values (0.8–1.2) that are indicative of anticlustered to weakly clustered patterns, particularly in the vein stockwork of
the upper part of the Golden Cross deposit. These Cv values are consistent with field observations that joints are a major control on vein spacing. In the poorly jointed dacitic
and rhyolitic rocks, the veins are weakly to strongly clustered as shown by higher Cv values (1.2–2.4), and are commonly associated with normal faults. Overall, andesite lava and dacite porphyry and pyroclastics
host thicker and more persistent veins than rhyolite lava and tuff. These larger veins contain significant volumes of high-grade
gold mineralisation. The higher chemical reactivity to hydrothermal fluids of andesite and dacite compared with rhyolite may
have aided propagation and thickening of the veins in andesite-hosted deposits. Within an individual epithermal deposit, location
close to thick veins, representing major fluid conduits, commonly overrides the effect of different lithologies. Sites that
are deeper and located within or adjacent to major vein structures have higher average vein thickness, percentage extension
and degree of vein clustering. Systematic collection and analysis of vein spacing, thickness and density data can be used
to define trends that are useful in the exploration of gold-bearing epithermal vein deposits.
Received: 25 August 1998 / Accepted: 23 December 1999 相似文献
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It is well known that the interaction of an interplanetary coronal mass ejection (ICME) with the solar wind leads to an equalisation
of the ICME and solar wind velocities at 1 AU. This can be understood in terms of an aerodynamic drag force per unit mass
of the form F
D/M=−(ρe
AC
D/M)(V
i−V
e)∣V
i−V
e∣, where A and M are the ICME cross-section and sum of the mass and virtual mass, V
i and V
e the speed of the ICME and solar wind, ρe the solar wind density, C
D a dimensionless drag coefficient, and the inverse deceleration length γ=ρe
A/M. The optimal radial parameterisation of γ and C
D beyond approximately 15 solar radii is calculated. Magnetohydrodynamic simulations show that for dense ICMEs, C
D varies slowly between the Sun and 1 AU, and is of order unity. When the ICME and solar wind densities are similar, C
D is larger (between 3 and 10), but remains approximately constant with radial distance. For tenuous ICMEs, the ICME and solar
wind velocities equalise rapidly due to the very effective drag force. For ICMEs denser that the ambient solar wind, both
approaches show that γ is approximately independent of radius, while for tenuous ICMEs, γ falls off linearly with distance.
When the ICME density is similar to or less than that in the solar wind, inclusion of virtual mass effects is essential. 相似文献
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Benoit Lavraud and Peter J Cargill explain the structure of the magnetospheric cusps and their relationship with the solar wind, as revealed by Cluster data. 相似文献
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The coupling of thermal and ideal MHD effects in a sheared magnetic field is investigated. A slab geometry is considered so that the Alfvén mode can be decoupled from the system. With the total perturbed pressure approximately zero, the fast mode is eliminated and a system of linearized equations describing magnetic effects on the slow mode and thermal mode is derived. These modes evolve independently on individual fieldlines. One of the main features of this approach is that the influence of the dense photosphere can be included. A variety of different conditions that simulate the photospheric boundary are presented and the different results are discussed. A choice of field geometry and boundary conditions is made which removes mode rational surfaces so that there are no regions in which parallel thermal conduction can be neglected. This provides a stabilizing mechanism for the thermal mode. Growth rates are reduced by 30–40% and there is complete stabilization for sufficiently short fieldlines. The influence of dynamic and thermal boundary conditions on the formation of prominences is discussed. 相似文献
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Peter J. Cargill 《Solar physics》1996,167(1-2):267-279
Spectral line profiles associated with the nanoflare model of coronal heating are computed. It is shown that the reconnection jets associated with this heating model lead to Doppler shifts or line broadening of coronal spectral lines in excess of those observed. Some possible resolutions of the problem are suggested. 相似文献
10.
The heating of post-flare loops in the Kopp-Pneuman (1976) model is here reconsidered. In that kinematic model the loops are heated by gas-dynamic shocks to at most 3–4 × 106 K. However, in a full dynamic model they would be replaced by slow magnetohydrodynamic shocks, which may provide more heating due to the additional release of magnetic energy. It is shown from a local compressible analysis that such shock waves can account for the observed temperatures of 5 × 106–107 K and also for the observed upward loop speeds of 1–50 km s-1. The above values are obtained when the ambient plasma beta is 0.01 and the shocks propagate at highly sub-Alfvénic velocities. However, if the velocity of shock propagation approaches the Alfvén speed, then temperatures of 108 K are produced. This may explain the extremely high temperatures that have been observed with the Solar Maximum Mission, when it is realised that the post-flare loop phenomenon may well be occurring very early on in the flare.A full dynamic model would require a sophisticated numerical computation, and so a simple global analytic model is developed here instead. It is incompressible and includes a strong solar-wind inflow along the reconnecting field lines. As the upflow increases, the loops become more compressed and the Alfvén waves approach one another. 相似文献