Topographic Comparisons of Uplift Features on Venus and Earth

Details Topographic Comparisons of Uplift Features on Venus and Earth Topographic Comparisons of Uplift Features on Venus and Earth

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p43d1704s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P43D-1704

Physics

[5475] Planetary Sciences: Solid Surface Planets / Tectonics, [5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6295] Planetary Sciences: Solar System Objects / Venus, [8148] Tectonophysics / Planetary Volcanism

Scientific paper

Venus and Earth display different hypsography. We use topographic profiles to search for well-understood terrestrial analogs to Venusian uplift features. Specifically, by using cross-correlation, we correlate average profiles for terrestrial rifts (slow and fast, "ultra-slow," incipient and inactive) and also hotspots (oceanic and continental) with those for Venusian chasmata and regiones, to draw inferences as to the processes responsible for shaping Venus' surface. Correlations tend to improve with faster spreading rates; Venus' correlations rank considerably lower than terrestrial ones, suggesting that if chasmata are analogous to terrestrial spreading centers, then spreading on Venus barely attains ultra-slow rates. Individual features' normalized average profiles are correlated with profiles of other such features to establish the degree of similarity, which in turn allows for the construction of a covariance matrix. Principal component analysis of this covariance matrix shows that Yellowstone more strongly resembles Atla, Beta and W. Eistla regiones than it does the terrestrial oceanic hotspots, Reunion and Hawaii. This analysis also shows that Venusian chasmata, especially Ganis, most closely resemble the ultra-slow spreading Arctic ridge.

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