Formation of Ishtar Terra, Venus: Surface and gravity constraints

Details Formation of Ishtar Terra, Venus: Surface and gravity constraints Formation of Ishtar Terra, Venus: Surface and gravity constraints

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995geo....23..292h&link_type=abstract

Geology, vol. 23, Issue 4, p.292

Computer Science

16

Scientific paper

We examine the geology of Ishtar Terra, Venus, as viewed in high-resolution Magellan synthetic-aperture radar imagery and altimetry, in order to interpret regional surface strain patterns. We combine constraints imposed by the surface strain with gravity modeling of Magellan degree-75 high-resolution gravity data. Long-wavelength (>2500 km) and short-wavelength (500 2500 km) features show different apparent depths of isostatic compensation. Ishtar straddles a long-wavelength topographic bulge that is compensated at ˜130 ± 40 km depth, whereas the short-wavelength features (individual mountain belts and tesserae) are compensated at varying depths in a range of ˜25 70 km. These two ranges of compensation, taken together with surface strain patterns, lead us to postulate a new model for the evolution of Ishtar Terra. In the model, mantle downflow results in ponding and thickening of partial melt residuum that compensates the long-wavelength bulge of Ishtar Terra. Thickened lower crust, resulting from shear forces associated with structurally deeper residuum, isostatically compensates short-wavelength topography. Relative displacement of the lower crust beneath the upper crust, which deforms in ruglike fashion, results in the surface strain patterns.

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