Volcanic rises on Venus: Geology, formation, and sequence of evolution

Details Volcanic rises on Venus: Geology, formation, and sequence of evolution Volcanic rises on Venus: Geology, formation, and sequence of evolution

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24.1279s&link_type=abstract

In Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z p 1279-1280 (SEE N94-20636 05-91

Physics

Geophysics

Equatorial Regions, Highlands, Planetary Geology, Tectonics, Venus (Planet), Venus Surface, Volcanoes, Volcanology, Geophysics, High Resolution, Imaging Techniques, Radar Imagery, Topography

Scientific paper

Large centers of volcanism on Venus are concentrated primarily in the equatorial region of the planet and are associated with regional topographic rises. Analysis of both radar images and geophysical data suggest that these uplands are sites of mantle upwelling. Magellan radar imaging provides a globally contiguous data set from which the geology of these regions is evaluated and compared. In addition, high resolution gravity data currently being collected provide a basis to assess the relationship between these uplands and processes in the planet's interior. Studies of the geology of the three largest volcanic highlands (Beta Regio, Atla Regio, Western Eistla Regio) show them to be distinct, having a range of volcanic and tectonic characteristics. In addition to these large areas, a number of smaller uplands are identified and are being analyzed (Bell Regio, Imdr Regio, Dione Regio (Ushas, Innini, and Hathor Montes), and Themis Regio). To understand better the mechanisms by which these volcanic rises form and evolve, we assess their geologic and geophysical characteristics.

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