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  • 1
    Electronic Resource
    Electronic Resource
    Amsterdam : Elsevier
    Advances in Space Research 9 (1989), S. 143-146 
    ISSN: 0273-1177
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics , Physics
    Type of Medium: Electronic Resource
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  • 2
    ISSN: 0273-1177
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics , Physics
    Type of Medium: Electronic Resource
    Library Location Call Number Volume/Issue/Year Availability
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  • 3
    Electronic Resource
    Electronic Resource
    Amsterdam : Elsevier
    Advances in Space Research 10 (1990), S. 71-73 
    ISSN: 0273-1177
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics , Physics
    Type of Medium: Electronic Resource
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  • 4
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 49 (1990), S. 57-83 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract The conclusion that the different ridge belt-bounded planitia and parquet terrains studied here define Venusian crustal plate-like units is evidently valid in the context of compressional ridge belt tectonics. The long ridge belts of Kamari and Tellus Dorsa, the ridge belts in the transition zone between Ishtar Terra and planitiae and Ausra Dorsa support the idea of NW-SE, (N-S) or E-W compression components, respectively. The planitia plates have been pushed from the south or south-east against the Ishtar Terra/Fortuna Tessera highland, which has opposed the movement, giving the impression of a relative southeast-directed force. The volcanic/diapiric transition zone between these colliding crustal units or plates evidently indicates mobilization of the subsurface unit overthrust by the parquet terrain.
    Type of Medium: Electronic Resource
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  • 5
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 73 (1996), S. 195-214 
    ISSN: 1573-0794
    Keywords: Venus ; impact craters
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract This article presents fractal analyses of 28 outflow margins from 18 Venusian impact craters. The fractal dimensions of the second parts of R-plots of the outflow outlines were measured by a three-step method. The fractality values for the same outflow measured from images which have only a small difference in resolution are very similar, while large differences in image resolution may result in differences in fractality, possibly due to the fact that we are actually studying geological processes on different scales. The outflows were classified into three general categories: single outflows, multiple outflows and outflow fields. Three conclusions were drawn on the relations between fractality and crater diameter, which may be related to the greater effects caused by the immediate local environment on the outflows from small craters than on those from larger craters. Investigation of the relations between the regional topography and fractality indicates that there are substantially less effects on outflows originating from large craters than on those from small craters. The smooth bending in the R-plot and the higher D-value for the multiple outflows could result from the mixing of various fractal or non-fractal units. When comparing our results with the fractality of terrestrial lava flows, outflows from craters of diameter greater than 50 km seem to resemble a′a-type lava flows in their fractal dimensions and outflows from craters of diameter below 50 km tend to be more pahoehoe-like. This preliminary result is based on 28 outflows, however, and the pattern should be investigated more carefully by further more extensive work.
    Type of Medium: Electronic Resource
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  • 6
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 74 (1996), S. 191-214 
    ISSN: 1573-0794
    Keywords: Planetary tectonics ; Venus
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract The intrablock deformation of Meshkenet Tessera on Venus is mostly due to responses of the uppermost surface bedrock to tensional stresses. It is found that complex deformation structures within the highland blocks resemble those of formed in chocolate tablet boudinaging which has taken place after original parallel faulting and bar-like crustal block formation. The high-angle tessera structures with varying cross-cutting relations define styles and locations of multiphase deformation most evidently related to local relaxation of tessera topography. Series of progressive or superposed fracturing events with alternating fault directions took place at high angles during this relaxational deformation. Compressional ridges often surround these tesserae.
    Type of Medium: Electronic Resource
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  • 7
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 58 (1992), S. 65-78 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Wrinkle ridge systems within and around Martian highland craters were studied in order to find their basin-induced and regional aspects. Most prominent ridge directions indicate regional tectonic patterns. Radial ridges near large craters are often slightly deflected along regional or global ridge systems. Crater floor ridges have simpler local distributions. Smaller or older craters are less resistant against the effects of global or regional stress systems. In craters concentric ridge rings locate at 0.8 crater radius with additional minor rings at 0.66, 0.44 and 0.94 crater radius. This pattern illustrates compression of lava fill over buried topography.
    Type of Medium: Electronic Resource
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  • 8
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 65 (1994), S. 55-70 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract The lengthy Meshkenet Tessera highland located between Ishtar Terra and coronae of the Nightingale group provides evidence of large-scale crustal movements. Its complex tectonic structures have various deformation geometries, thus indicating different tectonic sequences. The main parallel faults, first explained as rotational bookshelf faults, are more likely due to relative dextral direct shear movements of rectangular blocks. These faults have been active, possibly due to endogenic stresses, as indicated by mid-size ridge ranges which connect them to some of the large coronae. There are some compressional ridge belts around Meshkenet Tessera, while deformation within the tessera blocks has mostly been extensional.
    Type of Medium: Electronic Resource
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  • 9
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 19 (1978), S. 457-477 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract A structural analysis is presented of mare ridges in an area of about 360000 km2 in the southeastern part of Oceanus Procellarum just north of Mare Humorum. Mare ridges can be regarded as the result of large-scale natural tectonic deformation experiments coupled with and extended by volcanic phenomena. The old lunar crust has evidently retained part of the Moon's original tectonic elements throughout major exo- and endogenic events. Those structures which in places were flooded by mare lavas were also the first flaws to yield and to extend during younger tectonic and volcanic activity. Linear mare ridges may thus have formed at the activated and re-activated junctures of lunar crustal plates. Implications for the tectonics of mare ridges evidently show that one global stress field cannot account for all lunar tectonics but that global and areal variations in the lunar stress system have probably occurred.
    Type of Medium: Electronic Resource
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  • 10
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 19 (1978), S. 513-517 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Most recent tectonically notable lunar surface structures, straight or arcuate rilles and mare ridges are found to form regional lineament sets which are interpreted to be manifestations of crustal zones of weakness. The activity of the zones of weakness and their different parts range over a long period of time. Some parts of these zones may have undergone similar development to those of both experimental and natural strike-slip shears. It is hypothesized that the clearly discernable surface zone, which runs from the crater Lansberg to the crater Palmieri tangential to Mare Humorum, may coincide with a major moonquake belt described by Lammlein (1977).
    Type of Medium: Electronic Resource
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