THE THIN CRUST OF CIVILIZATION:

Author(s):  
MATHIAS BEREK
Keyword(s):  
1886 ◽  
Vol 3 (1) ◽  
pp. 11-12
Author(s):  
W. S. Gresley

During the summer of 1885, in excavating for a small reservoir for colliery purposes at Moira, three miles west of Ashby-de-la Zouch, au interesting deposit of a kind of Limonite Iron-ore was met with, the following description of which may interest some of the readers of the Geological Magazine.The bed occurred about five feet below the surface soil, near a small stream, at a place called “Hanging Hill” [see Geol. 1-inch Map, Quarter-Sheet No. 63, N.W.]. In thickness it hardly reached a foot, but its extent was not proved; it rested unconformably upon stiff blue clay of the Coal-measures, and was overlaid by yellowish clay, loam, sand, etc., unstratified, containing a few pebbles and other drifted matter; it was principally composed of nodules and fragments of nodules of earthy yellowish brown ironstone, of similarly formed pieces of very hard and compact light grey siliceous stone having a thin crust or shell of compact dark brown iron-ore, (probably göthite), of sandy nodular masses largely composed of limonite; of fragments and small nodules of fossiliierous hard red hæmatite generally coated with a bright red skin which is often powdery; also specimens of compact brown iron ore having a yellow ochre coating, sometimes the compact red and yellow hæmatites are associated in the same sample, the latter variety appears to form a kind of shell to the red ore, though occasionally the two kinds exist in thin alternating bands.


2021 ◽  
Vol 9 (2) ◽  
pp. T507-T521
Author(s):  
Camille Le Magoarou ◽  
Katja Hirsch ◽  
Clement Fleury ◽  
Remy Martin ◽  
Johana Ramirez-Bernal ◽  
...  

Rifts and rifted passive margins are often associated with thick evaporite layers, which challenge seismic reflection imaging in the subsalt domain. This makes understanding the basin evolution and crustal architecture difficult. An integrative, multidisciplinary workflow has been developed using the exploration well, gravity and magnetics data, together with seismic reflection and refraction data sets to build a comprehensive 3D subsurface model of the Egyptian Red Sea. Using a 2D iterative workflow first, we have constructed cross sections using the available well penetrations and seismic refraction data as preliminary constraints. The 2D forward model uses regional gravity and magnetic data to investigate the regional crustal structure. The final models are refined using enhanced gravity and magnetic data and geologic interpretations. This process reduces uncertainties in basement interpretation and magmatic body identification. Euler depth estimates are used to point out the edges of high-susceptibility bodies. We achieved further refinement by initiating a 3D gravity inversion. The resultant 3D gravity model increases precision in crustal geometries and lateral density variations within the crust and the presalt sediments. Along the Egyptian margin, where data inputs are more robust, basement lows are observed and interpreted as basins. Basement lows correspond with thin crust ([Formula: see text]), indicating that the evolution of these basins is closely related to the thinning or necking process. In fact, the Egyptian Northern Red Sea is typified by dramatic crustal thinning or necking that is occurring over very short distances of approximately 30 km, very proximal to the present-day coastline. The integrated 2D and 3D modeling reveals the presence of high-density magnetic bodies that are located along the margin. The location of the present-day Zabargad transform fault zone is very well delineated in the computed crustal thickness maps, suggesting that it is associated with thin crust and shallow mantle.


2021 ◽  
Vol 228 (1) ◽  
pp. 631-663
Author(s):  
Kyle Batra ◽  
Bradford Foley

SUMMARY Stagnant-lid convection, where subduction and surface plate motion is absent, is common among the rocky planets and moons in our solar system, and likely among rocky exoplanets as well. How stagnant-lid planets thermally evolve is an important issue, dictating not just their interior evolution but also the evolution of their atmospheres via volcanic degassing. On stagnant-lid planets, the crust is not recycled by subduction and can potentially grow thick enough to significantly impact convection beneath the stagnant lid. We perform numerical models of stagnant-lid convection to determine new scaling laws for convective heat flux that specifically account for the presence of a buoyant crustal layer. We systematically vary the crustal layer thickness, crustal layer density, Rayleigh number and Frank–Kamenetskii parameter for viscosity to map out system behaviour and determine the new scaling laws. We find two end-member regimes of behaviour: a ‘thin crust limit’, where convection is largely unaffected by the presence of the crust, and the thickness of the lithosphere is approximately the same as it would be if the crust were absent; and a ‘thick crust limit’, where the crustal thickness itself determines the lithospheric thickness and heat flux. Scaling laws for both limits are developed and fit the numerical model results well. Applying these scaling laws to rocky stagnant-lid planets, we find that the crustal thickness needed for convection to enter the thick crust limit decreases with increasing mantle temperature and decreasing mantle reference viscosity. Moreover, if crustal thickness is limited by the formation of dense eclogite, and foundering of this dense lower crust, then smaller planets are more likely to enter the thick crust limit because their crusts can grow thicker before reaching the pressure where eclogite forms. When convection is in the thick crust limit, mantle heat flux is suppressed. As a result, mantle temperatures can be elevated by 100 s of degrees K for up to a few Gyr in comparison to a planet with a thin crust. Whether convection enters the thick crust limit during a planet’s thermal evolution also depends on the initial mantle temperature, so a thick, buoyant crust additionally acts to preserve the influence of initial conditions on stagnant-lid planets for far longer than previous thermal evolution models, which ignore the effects of a thick crust, have found.


1963 ◽  
Vol 53 (1) ◽  
pp. 151-165
Author(s):  
Tetsuo A. Santô ◽  
Markus Båth

Abstract The dispersion of Rayleigh waves along a great number of Pacific paths has been studied by means of records from Pasadena, California, U. S. A., and Huancayo, Peru. Combining these measurements with previous ones based on records at Tsukuba, Hongkong, Honolulu and Suva, it was found that the central part of the Pacific Ocean exhibits the most oceanic structure, with exception for the Hawaiian Islands. In the south-eastern Pacific Ocean an area could be delineated with a new type of dispersion characteristics, not found in any other part of the Pacific. This area agrees closely with the Easter Island Ridge system, and exhibits unusually thin crust and low upper-mantle velocities as well as exceptionally high heat flow.


2016 ◽  
Vol 66 ◽  
pp. 1-14 ◽  
Author(s):  
María Laura Rosa ◽  
Bruno Collaço ◽  
Marcelo Assumpção ◽  
Nora Sabbione ◽  
Gerardo Sánchez

2000 ◽  
Vol 37 (2-3) ◽  
pp. 291-306 ◽  
Author(s):  
J Martignole ◽  
A J Calvert ◽  
R Friedman ◽  
P Reynolds

Results of deep seismic reflection survey along a 375 km long transect of the Grenville Province in western Quebec are combined with a review of geological observations and published isotopic ages. The seismic profile offers a remarkably clear image of the crust-mantle boundary and a good definition of the various crustal blocks. Crust about 44 km thick beneath the Grenville Front zone thins abruptly to ca. 36 km southeastward, perhaps the result of extension on southeast-dipping surfaces extending to the Moho. Other zones of relatively thin crust, although less pronounced, occur where Proterozoic crust overlies Archean crust, and beneath the Morin anorthosite complex. The thickest crust is found at the extreme southeast of the transect, east of the Morin anorthosite. From northwest to southeast, three main crustal subdivisions are (1) deformed Archean rocks with southeast-dipping reflectors in the Grenville Front zone, (2) an Archean parautochthon with northwest-dipping reflectors extending to the lower crust, and (3) an overlying three-layer crust interpreted as accreted Proterozoic terranes. The boundary between (2) and (3) is a major, southeast-dipping, crustal-scale ramp (Baskatong ramp) interpreted to have accommodated strain during and after accretion. U-Pb and Pb-Pb ages on detrital zircons show that metasedimentary rocks of the allochthons (Mont-Laurier, Réservoir Cabonga, and Lac Dumoine terranes) range from Archean to as young as 1.21 Ga. A single zone with 1.4 Ga old Sm-Nd model ages appears to lack Archean components and may be considered as a fragment of juvenile Mesoproterozoic crust pinched in a shear zone (Renzy shear zone) that could be raised to the status of terrane (Renzy terrane). In the allochthons, U-Pb ages of metamorphic zircon and monazite cluster around 1.17 Ga (Mont-Laurier and Réservoir Cabonga terrane) and 1.07 Ga (Renzy and Lac Dumoine terrane) and are interpreted to record late and post-accretion crustal reworking, a common feature of the Grenville orogen. A final high-grade metamorphic event (ca. 1.0 Ga) documented only in the parautochthon and the Grenville Front zone records large-scale, piggyback-style thrusting of allochthonous slabs onto the parautochthon. The age of transcurrent displacement following peak metamorphism affecting both the allochthons and the parautochthon decreases northwestward from 1.07 to 1.00 Ga. Dating thus shows that Grenvillian deformation in western Quebec occurred in pulses over an interval of 180 million years, with a tendency to propagate from the inner part of the orogen toward the Grenville Front. Reworked migmatites from the parautochthon cooled from the ca. 1.0 Ga peak of metamorphism through about 450°C (Ar closure in hornblende) at ca. 0.96 Ga with calculated cooling rates of about 6°C per million years, and unroofing rates of 0.33 km per million years. The cooling-unroofing history of the allochthons is not so straightforward, probably due to tectonic disturbances related to allochthon emplacement. Cooling through 450°C occurred between 1.04 and 1.01 Ga, at least 50 million years earlier than cooling in the parautochthon; this contrast agrees with the northwestward propagation of the orogen.


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