T184 Sedimentary Landscapes across the Solar System: Planets, Moons, and Terrestrial Analogues I
Thursday, 29 October 2020
10:00 AM - 12:00 PM
Meeting Rooms
MUD MEANDER MORPHODYNAMICS ON EARTH AND MARS
Paper number: T184-6
Program: Technical Sessions
Time: 11:05 AM – 11:20 AM
Authors
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Runze MiaoUniversity of California, Berkeley, Berkeley, CA
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William E. DietrichUniversity of California, Berkeley, Berkeley, CA
Abstract
In the Spring of 2017, we measured the velocity field and suspended sediment at one cross-section and the velocity field through a sequence of cross-sections through a tight bend. A rainstorm during the field work generated local runoff, raising the concentration of the flow, but not significantly the discharge. Migrating ripples of flocculated mud developed along the inner bank of a bend. This revealed that bands of mud-rich layers may record temporal change in mud input from local sources. To explore the conditions leading to inner bank mud accretion, we modified (in Delft3D) the use of standard cohesive entrainment and deposition models by assigning flocculated settling velocities to the mud and by including the sand fraction with the cohesive entrainment (as mud and sand are always co-deposited). A non-dimensional ratio of shear stress to a deposition function delineated areas of predicted erosion and deposition by grain size. Sandy mud is predicted to be deposited in active currents where the boundary shear stress-driven entrainment is less than the local settling velocity- concentration product. Post deposition drainage and consolidation leads to strengthening sufficient to slow erosion once these deposits are exposed to channel shifting, thereby sustaining river meandering in the absence of vegetation.
Geological Society of America Abstracts with Programs. Vol. 52, No. 6
doi: 10.1130/abs/2020AM-355190
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