Mathematics – Logic
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...p31a08s&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #P31A-08
Mathematics
Logic
5415 Erosion And Weathering, 5464 Remote Sensing, 5480 Volcanism (8450)
Scientific paper
Late-stage volcanic activity along the northwest flank of the Elysium volcanic construct deposited a variably fluidized sequence of channelized debris flows, in some cases >1500 km long, into Utopia Planitia. Using integrated imagery and topographic datasets, we have re-examined the stratigraphic relationships of these channelized deposits to help elucidate their history and evolution. Source troughs and chaotic depressions developed from differential heating along distributed patterns of pre-existing structures. Concentrated heating and intrusion along these structures caused collapse and mobilization of debris into laharic flows. Volumetric comparisons suggest that depressions within source terrains (Elysium Fossae and Galaxias Chaos/Fossae) inadequately account for the deposit volume. Though the volumes removed from the flanks of Elysium Mons regionally exceed 104 km3, the channelized deposits comprise >6x104 km3 as determined by cut/fill relations. These comparisons suggest the incorporation of substantial amounts of juvenile volcanic material while the lengthy run-out, smooth floors, and lobate terminations within the channelized deposits point to emplacement of highly fluidized debris. We are currently investigating the supplying relationships between the relatively shallow ( ~300 meters) northern source fossae and chaos and the topographically unconnected and considerably deeper troughs ( ~3000 meters) of Elysium Fossae in the south. We recognize subtle variations in morphologic styles between the southern and northern channelized flow deposits. Both deposits display extensive smooth medial floors bound by higher standing rugged terrains, which apparently acted as constructional "levees" constricting distribution into Utopia Planitia. However, potential pseudocraters, "softened" terrain, and discontinuous elevated channels suggest that the northern flows incorporated more volatile material and/or were emplaced upon volatile rich terrains. Regionally, the channelized terrains within Utopia Planitia likely formed by the interaction of magma with subsurface reservoirs of water, ice, and perhaps CO2, and variable incorporation of eroded debris. Both sequences of flows appear to be much younger than previously appreciated, as the ejecta of large impact craters are embayed and dissected by the flows and channels. Additionally, their surfaces are sparsely cratered in meter-resolution images, indicating that Mars has experienced significant volcanic/volatile interactions in geologically recent times.
Skinner Andrew J.
Tanaka Ken L.
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