Flow Emplacement Styles and Flow Rates From Flow Margin and Channel Topography: Examples From Terrestrial Field and Martian Altimetry Data

Details Flow Emplacement Styles and Flow Rates From Flow Margin and Channel Topography: Examples From Terrestrial Field and Martian Altimetry Data Flow Emplacement Styles and Flow Rates From Flow Margin and Channel Topography: Examples From Terrestrial Field and Martian Altimetry Data

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufm.v32a..02s&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #V32A-02

Physics

8429 Lava Rheology And Morphology, 8450 Planetary Volcanism (5480), 5464 Remote Sensing, 5480 Volcanism (8450), 6225 Mars

Scientific paper

Basaltic volcanism is the predominant volcanic mode for the terrestrial planets, and constraining basaltic emplacement styles and rates is key in estimating regional resurfacing rates, eruption durations, etc. In this study, we combine field and remote sensing data to constrain emplacement styles and eruption rates. For field approaches, we examine differential GPS topography profiles across terrestrial Eastern Snake River Plains (ESRP) basaltic flow margins to see if 1) flow surface type (e.g. pahoehoe. a'a, blocky, platy ) can be approximately determined from flow topography, 2) if flow emplacement modes (sheet flow, channel flow, tube flow, slow toe advance, etc.) can be constrained from topography and 3) model the apparent flow rate from the topography based on apparent flow emplacement mode. For remote sensing comparisons, we sample martian flows using Mars Orbiter Laser Altimeter (MOLA) , THEMIS (Thermal Emission Imaging System) and MOC (Mars Orbiter Camera) data. The MOLA profile data helps constrain emplacement styles with comparative flow margin topography and whole-flow cross-section profiles to detect tubes and channels. The THEMIS and MOC data are used in concert with MOLA data to constrain flow surface types. For the ESRP areas so far, the sub-meter sampling of flow margin profiles does constrain emplacement style (pahoehoe toe field, pahoehoe inflated, block pahoehoe, a'a), and that GPS channel topography yields good topographic constraints for flow rate modeling. In comparison, martian emplacement styles need both topography and images to adequately constrain flow surface type analogs due to the larger sampling spacing of the topography. However, many of the tube and channel flows are sufficiently large that the MOLA topography is sufficient for good flow rate modeling and constraints, and we find that ESRP calculated flow rates are quite similar to Cerberus region flow rates for Mars.

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