Formation of Venusian canali - Considerations of lava types and their thermal behaviors

Details Formation of Venusian canali - Considerations of lava types and their thermal behaviors Formation of Venusian canali - Considerations of lava types and their thermal behaviors

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9810873g&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. E6, p. 10,873-10,882.

Physics

45

Erosion, Fluid Flow, Heat Transfer Coefficients, Lava, Planetary Crusts, Venus Surface, Land Surface Temperature, Mathematical Models, Volcanoes, Venus, Channels, Origin, Formation, Lava Flow, Viscosity, Comparison, Komatiite, Basalt, Analysis, Model, Numerical Methods, Cooling, Fluid, Erosion, Theoretical Studies, Carbonatite, Sulfur, Calculations, Crust, Parameters, Thermal Effects, Mechanical Processes, Emplacement

Scientific paper

Because liquid water is unstable at present venusian surface conditions, the discovery of channels (termed 'canali') on Venus thousands of kilometers long was not predicted. Low viscosity lavas that remain fluid for several thousand kilometers are considered to be the canali-forming agents; possible compositions of Venusian canali-forming lavas include komatiite and high-Fe-Ti 'lunar'-type basalts. Results of analytical and numerical models of these lavas reveal that total cooling is more efficient on Venus than on Earth, suggesting that Venusian lavas rapidly form insulating crusts, and, thus, that the canali lavas were essentially 'tube-fed.' The models also reveal that thermal erosion should be less efficient on Venus than on Earth, suggesting that Venusian channels are either the product of mechanical (rather than thermal) erosion or constructional processes.

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