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  • 1
    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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  • 2
    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)
    Fulltext
  • 3
    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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  • 4
    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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    Paper (German National Licenses)
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  • 5
    Electronic Resource
    Electronic Resource
    Structures and activity of a lunar tectonic zone (1978)
    Springer
    Earth, moon and planets 19 (1978), S. 513-517 
    Details
    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
    URL: http://dx.doi.org/10.1007/BF00901977
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    Paper (German National Licenses)
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  • 6
    Electronic Resource
    Electronic Resource
    Tectonic implications of the mare-ridge pattern of the central parts of Oceanus Procellarum on the Moon (1980)
    Springer
    Earth, moon and planets 23 (1980), S. 307-321 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract A structural analysis is presented of the mare ridge pattern in an area of about 1 000 000 km2 in the central parts of Oceanus Procellarum. The penetration of magmas through the crust at the Marius Hills and Aristarchus Plateau/Harbinger Mountains volcanic complexes may have happened along pre-existing deep zone of weakness. Associated with these zones are present mare ridge ranges, some of which can be regarded as having formed radial or subradial ridge swarms to the complexes as they were strengthened by stress field changes caused by upward doming and penetrating magmas. The present moonquake epicentres within this area seem to be connected with mare ridge ranges. Focal depths from about 800 to 1000 km indicate a decreasing trend of tectonic activity. One shallow moonquake epicentre also lies within the mare ridge sets.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00902046
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    Paper (German National Licenses)
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  • 7
    Electronic Resource
    Electronic Resource
    Developments in the evaluation of small lake water quality from digital Landsat MSS data, Kuusamo, Northeast Finland (1984)
    Springer
    Earth, moon and planets 31 (1984), S. 249-264 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract The water quality data collected on the ground by the Water District Office in Oulu was subjected to statistical analyses together with Landsat data to display a few interactions and the possibilities of exploiting remote sensing methods in water area surveying. Correlations between the Landsat data statistics and some water quality measurements were identified. The small size of the studied lakes does not allow any clear calibration to be made but there could be possibilities to develop remote sensing methods for the evaluation of environmental variables and the detection of productivity and the eutrophication stage. The remote sensing procedure could also be useful in portraying temporal variations within lakes as well as relative variations between lakes by classifying each lake on a pixel-by-pixel basis. Although the remote sensing method is not able to supersede ground truth information for lake studies, it has value in regions where many lakes are to be found within a restricted small area. Under these circumstances the collection of information on the ground for a small number of test lakes and the generalization of this data, with the aid of machine-pressing remote sensing, would result in considerably less field work and cost savings.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00058904
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    Paper (German National Licenses)
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  • 8
    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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  • 9
    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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  • 10
    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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    Paper (German National Licenses)
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