Patterns of deformation and volcanic flows associated with lithospheric loading by large volcanoes on Venus

Details Patterns of deformation and volcanic flows associated with lithospheric loading by large volcanoes on Venus Patterns of deformation and volcanic flows associated with lithospheric loading by large volcanoes on Venus

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993thtp.nasas....m&link_type=abstract

In its Tectonic History of the Terrestrial Planets 1 p (SEE N94-31105 09-91)

Mathematics

Logic

Deformation, Finite Element Method, Geological Faults, Lithosphere, Loads (Forces), Radar Data, Radar Imagery, Tectonics, Topography, Venus (Planet), Venus Surface, Volcanoes, Altimetry, Annular Flow, Deposition, Elastic Plates, Erosion, Mathematical Models, Radial Flow, Sediments

Scientific paper

Magellan radar imaging and topography data are now available for a number of volcanoes on Venus greater than 100 km in radius. These data can be examined to reveal evidence of the flexural response of the lithosphere to the volcanic load. On Venus, erosion and sediment deposition are negligible, so tectonic evidence of deformation around large volcanoes should be evident except where buried by very young flows. Radar images reveal that most tectonic features and flow units on the flanks of these volcanoes have predominantly radial orientations. However, both Tepev Mons in Bell Regio and Sapas Mons in Atla Regio exhibit circumferential graben on their flanks. In addition, images reveal several flow units with an annular character around the north and west flanks of Tepev Mons. This pattern most likely results from ponding of flows in an annular flexural moat. Maat Mons in Atla Regio and Sif Mons in Eistla Regio are examples of volcanoes that lack circumferential graben and annular flows; discernible flow units and fractures on these constructs appear to be predominantly radial. Altimetry data can also provide evidence of flexural response. Tepev Mons is partially encircled by depressions that may be sections of a flexural moat that has not been completely filled. The locations of these depressions generally coincide with the annular flows described above. There is weaker evidence for such depressions around Maat Mons as well. The lack of circumferential tectonic features around most volcanoes on Venus might be explained by gradual moat filling and coverage by radial flows. The depressions around Tepev (and possible Maat) may indicate that this process is currently continuing. We use analytic models of plate flexure in an axisymmetric geometry to constrain the elastic plate thickness supporting Tepev Mons. If we consider the outer radius of the ponded flows to be the edge of a moat, we find that models with elastic plate thickness of 10-20 km fit best. Finite element models of a volcanic load detached from the underlying lithosphere predict overthrusting and radial normal faulting at the volcano's edge. Such a mechanism for the formation of radial rift zones on Venus volcanoes would make such features analogous to structures on the flanks of volcanoes on Earth.

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