Vulcanian explosive eruptions: A mechanism for localised pyroclast dispersal on Venus

Details Vulcanian explosive eruptions: A mechanism for localised pyroclast dispersal on Venus Vulcanian explosive eruptions: A mechanism for localised pyroclast dispersal on Venus

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..461f&link_type=abstract

In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F p 461-462 (SEE N94-12015 01-91)

Computer Science

Dispersing, Effusives, Ejection, Explosions, Extraterrestrial Environments, Gas Pressure, Magma, Venus (Planet), Volcanology, Vulcanizing, Compressed Gas, Earth Surface, Gas Composition, Rock Intrusions, Vents, Venus Atmosphere, Venus Surface

Scientific paper

A model of the mechanisms involved in transient (vulcanian-type) explosive eruptions has enabled us to place constraints on the velocities of blocks ejected during such events on Earth as well as on the excess pressure and concentration of gas in the vent prior to the onset of the explosion. This model, suitably modified, can predict the results of similar eruptions occurring under the differing Venusian environmental conditions. It is found that the much higher atmospheric pressure (approximately 100 bars at the mean planetary radius) dominates the form of the resulting deposit in two main ways: (1) by inhibiting the expansion out of the vent of overpressured gas, hence reducing ejecta velocity; and (2) by retarding the flight of ejected blocks via drag effects. Thus, it is expected that such deposits will typically extend to approximately 200 m on Venus as compared to several km for documented terrestrial deposits.

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