Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p22d..07s&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #P22D-07
Physics
6225 Mars, 8400 Volcanology, 8414 Eruption Mechanisms, 8450 Planetary Volcanism (5480)
Scientific paper
Recent advances in modeling of lava channels, lava tubes, and small edifice construction allow us to put more physically realistic constraints on effusion rates and rheologies. For this study, we combine these models with the new precise altimetry for Mars from the Mars Global Surveyor mission. The model suite includes solutions for Newtonian and Bingham rectangular channel flow, Newtonian and Bingham sheet flow, Newtonian and Bingham tube flow, and a percolation model for shield emplacement. We find that the new data and model accuracy allows us to apply these models for different flow regimes and regions to reveal probable differences in eruption rates or rheologies across Mars. Our estimations of effusions rates (for example) improve from a range of five to six orders of magnitude to a few, which allow possible discrimination of flow rate differences between regions of several orders of magnitude. Some, but not all, of the largest flow rates are found on the steepest slopes, but much of the variation is directly attributable to either effusion rate variations or rheology differences. We suggest that some of the differences are revealing characteristic eruption styles for specific martian regions, such as lower flow rates (after correction for different slopes) in Tyrrhena's flow field than are seen on the major shield volcanoes. However, some differences simply seem to reveal natural scatter within any given eruption style and model application. We will discuss results of models for several martian regions, and implications for regional and temporal changes in flow and effusion rate properties.
Gregg T. K.
Riedel S. J.
Sakimoto Susan E.
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