Venus banded terrain - Tectonic models for band formation and their relationship to lithospheric thermal structure

Details Venus banded terrain - Tectonic models for band formation and their relationship to lithospheric thermal structure Venus banded terrain - Tectonic models for band formation and their relationship to lithospheric thermal structure

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984jgr....89.6885s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 89, Aug. 10, 1984, p. 6885-6897. Research supported by the John Simon Gug

Astronomy and Astrophysics

Astronomy

63

Lithosphere, Planetary Temperature, Radar Astronomy, Tectonics, Terrain, Venus Surface, Planetary Crusts, Plates (Tectonics), Radar Imagery, Stress Analysis, Thickness, Viscosity, Venus, Terrain, Tectonism, Models, Bands, Formation, Lithosphere, Structure, Thermal Properties, Radar Observations, Imagery, Mountains, Istar Terra, Topography, Hypotheses, Features, Compression, Faulting, Extension, Folding, Plates, Elasticity, Viscosity, Depth, Thickness, Stress, Pressure, Wavelengths, Crust, Temperature

Scientific paper

Two classes of tectonic models for the formation of band structure on Venus mountain ranges are quantitatively evaluated: folding models and extensional models. The characteristics of banded terrain on Ishtar Terra are reviewed, particularly the evidence for a tectonic origin and such important details of band geometry as the spacing between adjacent bands. The tectonic models are tested against these observed features, and it it shown that both classes of models are possible explanations of banded terrain as long as the outer elastic-brittle layer of the Venus crust is at most a few kilometers thick. A general assessment is given of hypotheses for the origin of banded terrain and of the relationship between mechanical models for band formation and the thermal structure of the Venus lithosphere.

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