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Record Details

Record 14 of 11178
A Hybrid Model for Leveed Lava Flows: Implications for Eruption Styles on Mars
External Online Source: doi:10.1029/2008JE003278
Author and Affiliation:
Glaze, Lori S.(NASA Goddard Space Flight Center, Greenbelt, MD, United States)
Baloga, Stephen M.(Proxemy Research, Inc., Gaithersburg, MD, United States)
Garry, W. Brent(National Air and Space Museum, Center for Earth and Planetary Studies, Washington, DC, United States)
Fagents, Sarah A.(Hawaii Univ., Hawaii Inst. for Geophysics and Planetology, Honolulu, HI, United States)
Parcheta, Carolyn(Hawaii Univ., Hawaii Inst. for Geophysics and Planetology, Honolulu, HI, United States)
Abstract: Many cehannelized lava flows on the plains of Mars have substantial embanking margins and levees inferred to have been stationary while the central channel was active. Levee formation can be attributed to two end-member processes during emplacement; construction during passage of the flow front and growth along the entire length of the flow while it is active. It is shown here that the amount of lava that can be deposited by the flow front alone is limited. Estimates of the levee volume for many Mars plains flows exceed this limit and must have formed by processes that continued after the passage of the front. Experimental studies of analogous laboratory flows also indicate a combination of both modes of emplacement. A model that combines both modes of levee formation. is presented, including a method for estimating volumetric flow rate, eruption duration, and viscosity. Six lava flows on the plains of the Tharsis volcanic province are used as illustrative examples. Crustal thicknesses for the six flows examined range from 9 to 23 m. Estimated emplacement times required to cool crusts of these thicknesses range from I year to 10 years. Correspondini viscosities are on the order of 10 5-106 Pa s. Effusion rates range from 25 to 840 m 3 s - and are all within the range of terrestrial observations. Therefore, the large leveed plains flows on Mars are not dramatically different in eruption rate or lava viscosity from large terrestrial analogs.
Publication Date: Jan 01, 2009
Document ID:
20110007230
(Acquired Mar 11, 2011)
Subject Category: GEOPHYSICS
Document Type: Journal Article
Publication Information: Journal of Geophysical Research; Volume 114; E07001
Contract/Grant/Task Num: NNX06AD98G; NAG5-13348
Financial Sponsor: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Organization Source: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Description: 15p; In English; Original contains black and white illustrations
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: PLANETARY GEOLOGY; MARS VOLCANOES; FLOW VELOCITY; LAVA; MARS SURFACE; VISCOSITY; PLAINS; FLUID FLOW; ESTIMATES
Availability Source: Other Sources
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