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Zhamanshin
Examination of the topographic and orbital remote sensing signatures of two 10-km-class complex impact structures, Zhamanshin (Kazakhstan) and Bosumtwi (Ghana), both of which formed in the past 1 m.y., suggests either extreme differences in regional crater erosion rates during the Quaternary or some sort of fundamental difference in the preerosional topography of the structures. The visible to near-infrared spectral signature of the 14-km Zhamanshin feature is subtle, and is dominated by breccia and impact-glass covered hills apparently associated with the inner ring of a multiringed complex crater that formed only 870,000 years ago. The total dynamic range of relief at Zhamanshin is only 182 m, which is a factor of three less than that suggested from terrestrial crater scaling laws. By comparing typical 30 to 100 m spatial-resolution topographic cross sections for Zhamanshin and Bosumtwi, it is possible to assess the level of erosion that would be predicted at each structure over approximately 1 m.y., assuming each crater was formed with a preerosional morphology that can be reasonably approximated using existing terrestrial dimensional scaling relationships. It would apparently require at least an order of magnitude greater erosion at Zhamanshin to degrade the near-rim ejecta or to infill the crater interior to present-day levels than the erosional rate typical of the semi-desert sedimentary platform environment of this region of Kazakhstan. It is concluded that it is impossible to reconcile geologically plausible erosion rates at Zhamanshin with those required to infill and erode a typical 10 to 15 km complex impact crater to presently observed levels. Thus, we suggest that the preerosional morphology of Zhamanshin, unlike Bosumtwi, cannot be inferred using traditional complex crater scaling laws, and that Zhamanshin represents a new class of geologically subtle complex impact craters on the Earth whose initial morphology may reflect extreme late-stage slumping processes. It is possible that there may be tens of (relatively young) additional Zhamanshin-like complex craters within the sedimentary platforms on the continents, and that this as yet undetected population of impact features could help explain the observed deficiency of 10- to 20-km-diameter impact craters within the continental record (at least in the Cenozoic).
Zhamanshin crater, a possible source of Australasian tektites?
Comparison of the chemical composition of Zhamanshin and AATSF tektites on ...
Irghizites and microtektites from the Zhamanshin crater. A and C – dumb...
Geomorphologic scheme of Zhamanshin crater, according to [ 90 ] with supple...
Black, relatively uniform MN-tektites, comparable to lavas. 1 – layered t...
Nonuniform, layered Mn-tektites comparable with tuffiavas and multi-phase s...
Report of radiological ages of tektites of Australasian field (signs 1 an...
AUSTRALASIAN TEKTITES AND A GLOBAL DISASTER OF ABOUT 10,000 YEARS BP, CAUSED BY COLLISION OF THE EARTH WITH A COMET
Schematic map of distribution of tektites and impact craters related to the...
Abstract This account covers the history of tektites, from prehistoric times, through the descriptions by the Chinese in medieval times, their discovery and description in the Austro-Hungarian Empire in the 18th century, Charles Darwin’s encounter with a flanged button australite at what is now Albany, Western Australia, in the early 19th century, and the descriptions by Lacroix and others of further discoveries in Indo-China, the Ivory Coast and the USA, in the first half of the 20th century. F.E. Suess and R.H. Walcott first suggested a meteoritic provenance about 1900, and L.J. Spencer suggested ejection from terrestrial impact sites. Up to the 1950s, sophisticated research techniques were not available and speculation ruled, with many highly imaginitive and fanciful hypotheses emerging. As the Apollo landing approached, many new sophisticated research methods were developed and research proliferated. Evidence for terrestrial origin accumulated at this time, although lunar origin remained popular, and it was confirmed by rejection of lunar provenance following the Apollo and Luna recovery missions. The favoured mode of origin became ejection from a minority of large-scale impact sites on the Earth, and the relationship between the Ries impact structure and moldavites, and between Bosumtwi Crater and Ivory Coast tektites, was firmly established. Then in the 1990s the Chesapeake Bay structure was discovered, the source of the North American tektites? Wind-tunnel experiments by D.R. Chapman showed that flanged-button australites were produced by albation on descending through the atmosphere. Prolific researches, led by B.P. Glass, on deep-sea cores revealed the existence of microtektites, thus extending three of the strewn fields to large areas covered by sea. Kindred occurrences at Zhamanshin and Popigai in the USSR, in a Pliocene structure beneath the south Pacific Ocean, at the Cretacetus-Tertiary (K/T) boundary in Haiti and Mexico, and within late Devonian sediments in Belgium and China are briefly described, as well as natural glasses in Libya and Tasmania, of obscure origin. There remain a number of unsolved questions — among them the source of the huge Australasian Strewn Field, the enigma of the manner of dispersal of large, irregular Muong Nong-type tektites, the relationship of microtektites to the larger tektites found on land, and the relationship of all tektites to the geology of the likely target area of the source impact and processes of jetting from impact sites.
Is Ries crater typical for its size? An analysis based upon old and new geophysical data and numerical modeling
Considering the Ries crater as an example for middle-sized complex impact structures on Earth, we use geophysical data to examine the structure underneath the crater and simulate the formation process by numerical modeling. In contrast to previous investigations, we show by reanalyzing seismic refraction profiles that some clues for structural uplift exist beneath the crater in a range of at least 1 km. We propose that the average P-wave velocity inside the crater is lower than outside the crater from the surface to ∼2.2 km depth, but that below this level, the velocity increases beneath the center, presumably due to uplifted basement rocks. In addition, we utilized magnetotelluric depth sounding to investigate the deep electrical structure beneath the crater. Two-dimensional inversion models of the data show anomalously high conductivity beneath the crater. Our best model features a zone of presumably brine-filled fractures in open pore space to a depth of ∼2 km. Furthermore, our numerical modeling results for the crater formation are consistent with surface and subsurface observations in the vicinity of the crater. In order to explain the structural differences between similarly sized craters and Ries, we investigate the sensitivity of crater shape and subsurface structure to varying target compositions. We show that for a reasonable range of constitutive material and acoustic fluidization parameters the model calculations produce a large variety of different crater shapes, even for the same amount of impact energy. In contrast to the conventional estimate of crater diameters, our results suggest that Ries crater is comparable in size with the Bosumtwi and Zhamanshin crater. Despite their apparent lack of similarity at first look, Ries and Bosumtwi are closely matched in terms of transient crater size (inner ring), aspect ratio, and structural elements, and we conclude that they both represent typical complex crater structures of the terrestrial impact record for their size range.