A hybrid model for leveed lava flows: Implications for eruption styles on Mars

Details A hybrid model for leveed lava flows: Implications for eruption styles on Mars A hybrid model for leveed lava flows: Implications for eruption styles on Mars

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009jgre..11407001g&link_type=abstract

Journal of Geophysical Research, Volume 114, Issue E7, CiteID E07001

Physics

1

Planetary Sciences: Solid Surface Planets: Volcanism (6063, 8148, 8450), Planetary Sciences: Solar System Objects: Mars, Volcanology: Effusive Volcanism, Volcanology: Planetary Volcanism (5480, 6063, 8148), Volcanology: Lava Rheology And Morphology

Scientific paper

Many channelized lava flows on the plains of Mars have substantial embanking margins and levees inferred to have been stationary while the central channel was active. Levee formation can be attributed to two end-member processes during emplacement: construction during passage of the flow front and growth along the entire length of the flow while it is active. It is shown here that the amount of lava that can be deposited by the flow front alone is limited. Estimates of the levee volume for many Mars plains flows exceed this limit and must have formed by processes that continued after the passage of the front. Experimental studies of analogous laboratory flows also indicate a combination of both modes of emplacement. A model that combines both modes of levee formation is presented, including a method for estimating volumetric flow rate, eruption duration, and viscosity. Six lava flows on the plains of the Tharsis volcanic province are used as illustrative examples. Crustal thicknesses for the six flows examined range from 9 to 23 m. Estimated emplacement times required to cool crusts of these thicknesses range from 1 year to 10 years. Corresponding viscosities are on the order of 105-106 Pa s. Effusion rates range from 25 to 840 m3 s-1 and are all within the range of terrestrial observations. Therefore, the large leveed plains flows on Mars are not dramatically different in eruption rate or lava viscosity from large terrestrial analogs.

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