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Determining Emplacement Conditions and Vent Locations for Channelized Lava Flows Southwest of Arsia Mons by I. T. W. Flynn; D. A. Crown; M. S. Ramsey is a Physics and Astronomy article available to read on EtoBox.

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## Abstract The lava flow field southwest of Arsia Mons, Mars has complex volcanic geomorphology. Overlapping flows make observations of their total lengths and identification of their source vents impossible. Application of flow emplacement models, which rely upon physical parameters such as flow length, using only the exposed flow may produce inaccurate estimates of effusion rate, viscosity, and yield strength. We use an established terrestrial thermorheological model (PyFLOWGO), modified to Mars conditions, to estimate effusion rates, viscosities, yield strengths, and possible vent locations for five Mars flows. Our investigation found a range of effusion rates from 2,500 to 6,750 m^3^ s^−1^ (average of ∼4,960 m^3^ s^−1^). These results are an order of magnitude higher than terrestrial channelized basaltic flows. Corresponding modeled viscosities and yield strengths ranged from 9.4 × 10^3^ to 6.6 × 10^5^ Pa s (average of 5.5 × 10^4^ Pa s) and 66 to 381 Pa (average of 209 Pa), respectively. A novel secondary application of PyFLOWGO that assumes upslope channel narrowing provided estimates of the entire channel length, which is on average four times longer than the exposed portion

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Author

I. T. W. Flynn; D. A. Crown; M. S. Ramsey

Publisher

American Geophysical Union (AGU)

Published

2022

Language

EN

Field

Physics and Astronomy (Physical Sciences)