Le Havre—Antifer: a giant channel port     

Hugh Clout 《Geoforum》1975,6(3-4)

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A linear mathematical model for the seismic inplane behaviour of brick masonry walls part 1: Theoretical considerations     

Yalcin Mengi  Haluk Sucuolu  Hugh D. McNiven 《地震工程与结构动力学》1984,12(3):313-326

In this study two mathematical models are presented for the linear dynamic behaviour of masonry walls. The study is completed in three stages: experimental observations, selection of a mathematical model and the determination of model parameters through optimization analysis. In the present paper (Part 1) the theoretical analysis used in the development of the mathematical models is presented. Part 2 is devoted to the optimization analysis. Evaluation of the experimental data, which is described in detail in Part 2, indicates that the first two modal frequencies of the wall specimen are close to each other. This may be attributed, on physical grounds, to strong interaction between the brick and mortar phases of the wall. Accordingly, a two-phase mathematical model, namely a mixture model (MM), is chosen to describe the wall behaviour because it can differentiate between the two phases of the wall and take into account the interaction between them. The equations of MM are put into a discrete form to simplify the optimization analysis. As a special case, MM contains a simple one-phase model called the effective modulus model (EMM). The equations of EMM are also established. Finally, the theoretical complex frequency response functions (CFRF) predicted by MM and EMM are obtained. CFRF relates the top acceleration of the wall to its base acceleration and is the response quantity chosen to be matched in the optimization analysis.  相似文献   

An oxygen isotope study of hydrothermal alteration in the Lake City caldera, San Juan Mountains, Colorado     

Peter B. Larson  Hugh P. Taylor Jr. 《Journal of Volcanology and Geothermal Research》1986,30(1-2)

A 23-m.y.-old, fossil meteoric-hydrothermal system in the Lake City caldera (11 × 14 km) has been mapped out by measuring δ ¹⁸O values of 300 rock and mineral samples. δ ¹⁸O varies systematically throughout the caldera, reaching values as low as −2. Great topographic relief, regional tilting, and variable degrees of erosion within the caldera all combine to give us a very complete section through the hydrothermal system, from the surface down to a depth of more than 2000 m. The initial δ ¹⁸O value of the caldera-fill Sunshine Peak Tuff was very uniform (+7.2 ± 0.1), making it easy to determine the exact amount of ¹⁸O depletion experienced by each sample during hydrothermal alteration. Also, we have excellent stratigraphic control on depths beneath the mid-Tertiary surface, quantitative information on mineralogical alteration products, and accurate data on the shape of the central resurgent intrusion, which was the principal ‘heat engine’ that drove the hydrothermal circulation. Major conclusions are: (1) Although pristine mid-Tertiary meteoric waters in this area had δ ¹⁸O −14, these fluids were ¹⁸O-shifted upward to about δ¹⁸O = −8 to −5 prior to entering the shallow convective system associated with the resurgent intrusive rocks. Although there was undoubtedly radial inflow toward the caldera from all directions, the highly fractured Eureka Graben, southwest of the caldera, was probably the principal source of recharge groundwater for the Lake City system. (2) Fluid flow within the caldera was dominated by three major categories of permeable zones: the porous megabreccia units (which dip outward from the resurgent dome), vertical fractures and faults related to resurgence, and the caldera ring fault itself. All of these zones exhibit marked ¹⁸O depletions, and they are also typically intensely mineralogically altered. (3) The resurgent intrusive stock and its contact metamorphic aureole of hornfels both experienced water/rock ratios lower than the permeable zones; however, they have similarly low δ ¹⁸O values because they were altered at higher temperatures. (4) Throughout the caldera, the δ ¹⁸O of Sunshine Peak Tuff decreases with increasing depth (about 6 per mil/km), indicative of a shallow thermal gradient, typical of a convective hydrothermal system. The near-surface portion of this gradient was controlled by the temperature drop associated with boiling in the uprising fluid. (5) Deeply circulating meteoric water rose along permeable ring fractures 3 to 5 km beneath the mid-Tertiary surface. These fluids were drawn into the shallow convective system through the lower, porous, megabreccia units. Near the resurgent intrusions, fluid flow was again directed upward where resurgence-related, near-vertical fractures intersect the megabreccia units.  相似文献   

18O/16O ratios in ash-flow tuffs and lavas erupted from the central Nevada caldera complex and the central San Juan caldera complex,Colorado     

Peter B. Larson  Hugh P. Taylor Jr. 《Contributions to Mineralogy and Petrology》1986,92(2):146-156

Oxygen isotope compositions were measured on 129 quartz, feldspar, and biotite phenocrysts from ash-flow tuffs and lava domes erupted from the Oligocene central Nevada and central San Juan caldera complexes. Most of the ash-flow tuffs are compositionally zoned with low-phenocryst rhyolite bases and high-phenocryst quartz-latite tops, but both within individual units and throughout each of the eruptive sequences at each locality, the ¹⁸O values are remarkably constant. ¹⁸O values of the central Nevada magmas range from +9.1 to +9.8 per mil: These values are high and indicate the involvement of high-¹⁸O geosynclinal sediments in the melting process. Magmatic ¹⁸O values decrease by only about 0.4 per mil from the initial eruption sequence to the middle eruptive, the giant Monotony Tuff (3000 km³). The initial higher ¹⁸O values are reestablished in the late eruptive sequence, but decrease again by about 0.4 per mil in the latest ring-fracture eruptions. ¹⁸O values in the central San Juan magmas range from +6.8 to +7.5: These values are relatively low and indicate involvement of lower cratonal crust and upper mantle in the melting process. Magmatic ¹⁸O values decrease by about 0.4 per mil from the early sequence (Fish Canyon, Carpenter Ridge, and Mammoth Mountain Tuffs) to the late sequence (Wason Park, Nelson Mountain, and Snowshoe Mountain Tuffs). ¹⁸O/¹⁶O fractionations among phenocrysts in both Nevada and Colorado are much smaller than among corresponding minerals in plutonic granitic rocks. These fractionations also decrease from stratigraphically lower to higher samples in each cooling unit, so the ¹⁸O/¹⁶O data agree with other evidence that these represent quenched equilibrium at magmatic temperatures, and that prior to eruption the tops of the magma chambers were cooler than the deeper portions. In striking contrast to what is observed in Iceland and in the late-Tertiary to Quaternary southwest Nevada and Yellowstone caldera complexes, we have found no evidence for any low-¹⁸O rhyolitic magmas. Thus, low-¹⁸O rhyolitic magmas must be less common than heretofor believed, and their origin must be a result of special circumstances involving the timing, depth, and intensity of meteoric-hydrothermal activity. We tentatively suggest that extensional tectonics and regional rifting may be one of the prerequisites for their development.Contribution No. 4106, Publications of the Division of Geological and Planetary Sciences, California Institute of Technology  相似文献   

Downslope movement of in situ clasts on forested hillslopes,Virginia     

Hugh H Mills 《地球表面变化过程与地形》1986,11(4):451-456

Downslope movements of 109 clasts ranging in intermediate diameter from 30 to 870 mm were monitored over a five-year period on hillslopes in the Valley and Ridge province of southwest Virginia. Gradients ranged from 8° to 42°. Regression on slope tangent, depth of clast base below ground surface, clast size, and clast shape explained 70 per cent of clastmovement variance. A substantial part of the unexplained variance appears due to variation in substrate and slope aspect. Additional measurements made on two steep boulder streams showed extremely low rates.  相似文献   

Oxygen and hydrogen isotope studies of serpentinization in the Troodos ophiolite complex,Cyprus     

Mordeckai Magaritz  Hugh P. Taylor 《Earth and Planetary Science Letters》1974,23(1):8-14

Oxygen and hydrogen isotopic compositions were measured on 12 serpentine and 2 actinolite samples from the Troodos ophiolite complex, Cyprus. The single analyzed antigorite(δD= ?60, δ¹⁸O= 7.1) is isotopically similar to all previously analyzed antigorites from ultramafic bodies. However, although their D/H ratios are relatively “normal”(δD= ?70to?92), the δ¹⁸O values of most of the Troodos lizardite-chrysotile serpentines (+12.6 to +14.1) are much higher than the 2.0–9.3‰ range typically found in such serpentines. Such high δ¹⁸O values have previously been found only in the serpentine-like mineraloids termed “deweylites”, which apparently formed at Earth-surface temperatures, and in a single sample from Vourinos, Greece that is in contact with high-¹⁸O limestone. The Troodos lizardite-chrysotile samplescannot have formed by reaction with heated ocean waters, but instead must have formed in contact with large amounts of some type of meteoric, metamorphic, or formation water, either (1) at very low temperatures in a near-surface environment, or (2) at about 100°C from waters that were abnormally enriched in¹⁸O(δ¹⁸O ≈ +4 to +8). The latter possibility seems most plausible inasmuch as extensive evaporites were deposited throughout the Mediterranean Sea during the late Miocene, and this would have been accompanied by strong¹⁸O enrichments of the local meteoric waters. Heated ocean waters, however, probably were responsible for the formation of the actinolitic amphiboles(δ¹⁸O= 4.6 to 5.5; δD= ?51to?46) from the gabbro and ultramafic zones in the Troodos complex. The amphiboles must have formed at considerably higher temperatures and at an earlier stage than the lizardite-chrysotile serpentinization.  相似文献   

Microseism propagation via oceanic waveguide     

Hugh Bradner 《Pure and Applied Geophysics》1973,103(1):266-273

Summary Experiments have been made to determine whether a significant amount of microseism energy in the open ocean can be carried in organ-pipe waveguide modes. A three-component seismometer in a spherical aluminum container was balanced to float freely at midwater depth; a similar instrument was dropped on the ocean bottom. Simultaneous records from the two instruments were analyzed for peaks in coherence of their power spectra. Results indicate a substantial energy in modes in the ocean area of the observation, though the peak power appears in an unidentified mode with large horizontal motion of the water.Measurements at the same area, but widely separated in time, indicate that the frequencies of microseism peaks and the general shape of the microseism spectrum are characteristic of the geographicallocation, in agreement with the conclusion of Monakhov. The microseisms are characterized as motion in a wave guide that is excited by a non-white forcing function.  相似文献   

The structure of galaxy clusters in various cosmologies     

Peter A. Thomas  Jörg M. Colberg  Hugh M. P. Couchman  George P. Efstathiou  Carlos S. Frenk  Adrian R. Jenkins  Alistair H. Nelson  Roger M. Hutchings  John A. Peacock  Frazer R. Pearce  & Simon D. M. White 《Monthly notices of the Royal Astronomical Society》1998,296(4):1061-1071

We investigate the internal structure of clusters of galaxies in high-resolution N -body simulations of four different cosmologies. There is a higher proportion of disordered clusters in critical-density than in low-density universes, although the structure of relaxed clusters is very similar in each case. Crude measures of substructure, such as the shift in the position of the centre-of-mass as the density threshold is varied, can distinguish the two in a sample of just 20 or so clusters; it is harder to differentiate between clusters in open and flat models with the same density parameter. Most clusters are in a quasi-steady state within the virial radius and are well-described by the density profile of Navarro, Frenk & White.  相似文献   

Large-Scale Active Coronal Phenomena in Yohkoh SXT Images – IV. Solar Wind Streams from Flaring Active Regions     

Švestka  Zdeněk  FárnÍk  František  Hudson  Hugh S.  Hick  Paul 《Solar physics》1998,182(1):179-193

We demonstrate limb events on the Sun in which growing flare loop systems are embedded in hot coronal structures looking in soft X-rays like fans of coronal rays. These structures are formed during the flare and extend high into the corona. We analyze one of these events, on 28–29 August 1992, which occurred in AR 7270 on the eastern limb, and interpret these fans of rays either as temporary multiple ministreamers or plume-like structures formed as a result of restructuring due to a CME. We suggest that this configuration reflects mass flow from the active region into interplanetary space. This suggestion is supported by synoptic maps of solar wind sources constructed from scintillation measurements which show a source of enhanced solar wind density at the position of AR 7270, which disappears when 5 days following the event are removed from the synoptic map data. We also check synoptic maps for two other active regions in which existence of these fan-like structures was indicated when the active regions crossed both the east and west limbs of the Sun, and both these regions appear to be sources of a density enhancement in the solar wind. Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1005033717284  相似文献   

Large-scale active coronal phenomena in Yohkoh SXT images   总被引：1，自引：0，他引：1  

Zdenk vestka  Frantiek Fárník  Hugh S. Hudson  Yutaka Uchida  Paul Hick  James R. Lemen 《Solar physics》1995,161(2):331-363

We have found several occurrences of slowly rising giant arches inYohkoh images. These are similar to the giant post-flare arches previously discovered by SMM instruments in the 80s. However, we see them now with 3–5 times better spatial resolution and can recognize well their loop-like structure. As a rule, these arches followeruptive flares with gradual soft X-ray bursts, and rise with speeds of 1.1–2.4 km s^–1 which keep constant for >5 to 24 hours, reaching altitudes up to 250 000 km above the solar limb. These arches differ from post-flare loop systems by their (much higher) altitudes, (much longer) lifetimes, and (constant) speed of growth. One event appears to be a rise of a transequatorial interconnecting loop.In the event of 21–22 February 1992 one can see both the loop system, rising with a gradually decreasing speed to an altitude of 120 000 km, and the arch, emerging from behind the loops and continuing to rise with a constant speed for many more hours up to 240 000 km above the solar limb. In the event of 2–3 November 1991 three subsequent rising large-scale coronal systems can be recognized: first a fast one with speed increasing with altitude and ceasing to be visible at about 300 000 km. This most probably shows the X-ray signature of a coronal mass ejection (CME). A second one, with gradually decreasing speed, might represent very high rising flare loops. A third one continues to rise slowly with a constant speed up to 230 000 km (and up to 285 000 km after the speed begins to decay), and this is the giant arch. This event, including an arch revival on November 4–5, is very similar to rising giant arches observed by the SMM on 6–7 November 1980. Other events of this kind were observed on 27–28 April 1992, 15 March 1993, and 4–6 November 1993, all seen above the solar limb, where it is much easier to identify them.The temperature in the brightest part of the arch of 2–3 November 1991 was increasing with its altitude, from 2 to 4 × 10⁶ K, which seems to be an effect of slower cooling at lower densities. Under an assumption of line-of-sight thickness of 50 000 km, the emission measure indicates densities from 1.1 × 10¹⁰ cm^–3 at an altitude of 150 000 km to 1.0 × 10⁹ cm^–3 at 245 000 km 11.5 hours later. It appears that the arch is composed of plasma of widely different temperatures, and that hot plasma rises faster than the cool component. Thus the whole arch expands upward, and its density gradient increases with time, which explains whyYohkoh images show only the lowest and coolest parts of the expanding structure. The whole arch may represent an energy in excess of 10³¹ erg, and more if conduction contributes to the arch cooling.We suggest that the rise of the arch is initiated by a CME which removes the magnetic field and plasma in the upper corona, and the coronal structures remaining below this cavity begin to expand into the vacuum left behind the CME. However, we are unable to explain why the speed of rise stays constant for so many hours.  相似文献