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  • 1
    Electronic Resource
    Electronic Resource
    SIMS remote analysis of the Phobos surface: The DION experiment
    Amsterdam : Elsevier
    Advances in Space Research 10 (1990), S. 49-52 
    Details
    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
    URL: http://linkinghub.elsevier.com/retrieve/pii/0273-1177(90)90324-S
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Wrinkle ridges on mars
    Amsterdam : Elsevier
    Advances in Space Research 10 (1990), S. 71-73 
    Details
    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
    URL: http://linkinghub.elsevier.com/retrieve/pii/0273-1177(90)90329-X
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    Paper (German National Licenses)
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  • 3
    Electronic Resource
    Electronic Resource
    Development of the Alba Patera volcano on Mars
    Amsterdam : Elsevier
    Advances in Space Research 9 (1989), S. 143-146 
    Details
    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
    URL: http://linkinghub.elsevier.com/retrieve/pii/0273-1177(89)90220-2
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    Paper (German National Licenses)
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  • 4
    Electronic Resource
    Electronic Resource
    Ridge systems related to Martian impact craters (1992)
    Springer
    Earth, moon and planets 58 (1992), S. 65-78 
    Details
    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
    URL: http://dx.doi.org/10.1007/BF00058074
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    Paper (German National Licenses)
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  • 5
    Electronic Resource
    Electronic Resource
    Crustal tectonic zone on Venus (1994)
    Springer
    Earth, moon and planets 64 (1994), S. 155-164 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Various tectonic structures to the south and southeast of Ishtar Terra indicate areal stresses. Compression from east-southeast against Ishtar Terra has resulted in ridge belt formation and surface bending at Salme Dorsa, probably along the seam between two crustal units. En echelon fault zone indicates dextral strike-slip shear(s) resulted in the westward movement of planitia crust related to Ishtar Terra. Meshkenet Tessera displays differential dextral strike-slip faulting where the southernmost bar-like blocks have had largest relative movements. Compression against Tusholi Corona has resulted in foreland surface bending similar to that of Salme Dorsa. The tectonic zone as a whole resembles a dextral transform fault extending from a concave arc in the west to another concave arc in the east. The Cytherean surface, crust or uppermost lithosphere seems to be able to transmit stresses over distances. Deeper understanding of these processes is needed to gain a new idea of the crustal deformation on terrestrial planets.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00604487
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    Paper (German National Licenses)
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  • 6
    Electronic Resource
    Electronic Resource
    Main fault tectonics of Meshkenet Tessera on Venus (1994)
    Springer
    Earth, moon and planets 65 (1994), S. 55-70 
    Details
    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
    URL: http://dx.doi.org/10.1007/BF00572199
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  • 7
    Electronic Resource
    Electronic Resource
    Fractal properties of crater ejecta outlines on Venus (1995)
    Springer
    Earth, moon and planets 71 (1995), S. 9-31 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Fractal property or self-similarity exists abundantly in many aspects in our universe. Fractals are rich in geology and have certain relations to various geological processes. This article presents analyses of fractal properties of 18 impact crater ejecta margins on the surface of Venus. The structured walk method was used to measure the length of perimeter of the ejecta margin and the resulting Richardson plots were investigated. EveryR-plot has a first linear part, a second part and a main scattering part. The variations seen in the second part include information on the formation and geology of the crater ejectas. The fractal dimension of the second part is related to the perimeter of the ejecta and thus to the impact energy. The ratio of the square of the perimeter to the area describes the lobateness of the ejecta and has a positive correlation to the perimeter in a way similar to that between the fractal dimension of the second part and the perimeter. Two linear subparts in the second part indicate different fractal properties due to various processes dominating on different scales. Scattering in the middle of the second part indicates the scale and type of the ejecta lobes. The smooth scattering over the entire second part is related to impact angle and energy. A threshold value beyond which the structured walk method cannot be used was observed at a ruler length of about 1/10 of the perimeter.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00612866
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    Paper (German National Licenses)
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  • 8
    Electronic Resource
    Electronic Resource
    Chocolate tablet aspects of tectonics of Meshkenet Tessera on Venus (1996)
    Springer
    Earth, moon and planets 74 (1996), S. 191-214 
    Details
    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
    URL: http://dx.doi.org/10.1007/BF00055186
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  • 9
    Electronic Resource
    Electronic Resource
    Tectonic pattern of the Crüger/Rima Sirsalis -Rima de Gasparis region of the moon (1977)
    Springer
    Earth, moon and planets 17 (1977), S. 289-308 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Tectonic lunar units were studied in an area of about 540 000 km2 in the southwestern part of the Moon's visible disk. The area is situated in the vicinity of Mare Humorum, Oceanus Procellarum, and Mare Orientale. Zones indicated by lineament sets show three preferred orientations (about N55°W, N10°W, N35°E). Probably these zones coincide with deep faults that have been active over a long period of lunar development. The distribution of Eratosthenian and partly also Imbrian lavas coincides with the zones along which re-activations have taken place. This is best seen in the areas where strong zones intersect each other. Local catastrophic forces must also be taken into account. The trends, distribution, and age relations of tectonic zones can be explained by a combination of maximum principal stress in direction about N10°W coupled possibly with old tidal forces and local (?) volcanic expansion of lunar mantle during the last stages of flooding of Oceanus Procellarum.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00562201
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  • 10
    Electronic Resource
    Electronic Resource
    Tectonic pattern of mare ridges of the letronne-montes riphaeus region of the Moon (1978)
    Springer
    Earth, moon and planets 19 (1978), S. 457-477 
    Details
    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
    URL: http://dx.doi.org/10.1007/BF00901975
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