Mathematics – Logic
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p61d..04g&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P61D-04
Mathematics
Logic
5480 Volcanism (8450), 6225 Mars, 8400 Volcanology, 8429 Lava Rheology And Morphology
Scientific paper
Using the thermo-rheological model FLOWGO, we have considered the effects of Martian gravitational and environmental conditions on the cooling of lava flowing in a channel. Atmospheric temperature and density differences have only minor effects and the most significant effects are due to the differences in gravity between Earth and Mars: 1) the lower gravitational acceleration on Mars means that lava flows more slowly in a channel of a given size than it would on Earth; 2) this slower flow means that a more extensive insulating crust can form; 3) this more extensive crust reduces the cooling rate; and 4) slower flow also means a smaller volumetric flow rate (width x depth x velocity) if channel dimensions are equal. FLOWGO allows us to compare both temporally and spatially two flows of equal volumetric flow rate (but with the Martian channel necessarily larger than the Terrestrial one). If compared at the same time since leaving the vent, the more extensive crust on the Martian flow means that its core temperature will be higher. At the same distance from the vent, the Martian lava will have a more extensive surface crust but its core temperature will be lower. This is because it has taken longer to get there and therefore been cooling for a longer period of time. This means that if a Martian flow and a Terrestrial flow have the same length, the Martian flow was emplaced at a higher volumetric flow rate. That Martian flows are typically longer than Terrestrial flows means that their volumetric flow rates are considerably higher.
Garbeil Harold
Harris Jessica A.
Rowland Scott K.
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