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CO2 sublimation in Martian gullies: laboratory experiments at varied slope angle and regolith grain sizes
EC| UPWARDS ,
EC| EPN2020-RI
Sylvest, Matthew E.; Dixon, John C.; Conway, Susan J.; Patel, Manish R.; McElwaine, Jim N.; Hagermann, Axel; Barnes, Adam;
Sylvest, Matthew E.; Dixon, John C.; Conway, Susan J.; Patel, Manish R.; McElwaine, Jim N.; Hagermann, Axel; Barnes, Adam;
CO2 sublimation in Martian gullies: laboratory experiments at varied slope angle and regolith grain sizes
Martian gullies were initially hypothesized to be carved by liquid water, due to their resemblance to gullies on Earth. Recent observations have highlighted significant sediment transport events occurring in Martian gullies at times and places where CO2 ice should be actively sublimating. Here we explore the role of CO2 sublimation in mobilizing sediment through laboratory simulation. In our previous experimental work, we reported the first observations of sediment slope movement triggered by the sublimation of CO2 frost. We used a Mars regolith simulant near the angle of repose. The current study extends our previous work by including two additional substrates, fine and coarse sand, and by testing slope angles down to 10°. We find that the Mars regolith simulant is active down to 17°, the fine sand is active only near the angle of repose and the coarse sand shows negligible movement. Using an analytical model, we show that under Martian gravity motion should be possible at even lower slope angles. We conclude that these mass-wasting processes could be involved in shaping Martian gullies at the present day and intriguingly the newly reported CO2-creep process could provide an alternative explanation for putative solifluction lobes on Mars.
- University of Arkansas at Fayetteville United States
- Université Nantes
- Durham University United Kingdom
- Parthenope University of Naples Italy
- STFC Rutherford Appleton Laboratory United Kingdom
6417
ALLEN, C.C., MORRIS, R.V., KAREN, M.J., GOLDEN, D.C., LINDSTROM, M.M. & LOCKWOOD, J.P. 1998. Martian Regolith Simulant JSC Mars-1. Lunar and Planetary Science Conference XXVIII, 1690.
APPÉRÉ, T., SCHMITT, B. ET AL. 2011. Winter and spring evolution of northern seasonal deposits on Mars from OMEGA on Mars Express. Journal of Geophysical Research E Planets, 116, https://doi.org/10.1029/ 2010JE003762
AULD, K.S. & DIXON, J.C. 2016. A classification of Martian gullies from HiRISE imagery. Planetary and Space Science, 131, 88-101, https://doi.org/10.1016/j.pss. 2016.08.002
BALME, M.R., GALLAGHER, C.J. & HAUBER, E. 2013. Morphological evidence for geologically young thaw of ice on Mars: a review of recent studies using highresolution imaging data. Progress in Physical Geography, 37, 289-324, https://doi.org/10.1177/030913 3313477123
BARGERY, A.S., BALME, M.R., WARNER, N., GALLAGHER, C.J. & GUPTA, S. 2011. A background to Mars exploration and research. In: BALME, M.R., BARGERY, A.S., GALLAGHER, C.J. & GUPTA, S. (eds) Martian Geomorphology. Geological Society, London, Special Publications, 356, 5-20, https://doi.org/10. 1144/SP356.2
CEDILLO-FLORES, Y., TREIMAN, A.H., LASUE, J. & CLIFFORD, S.M. 2011. CO2 gas fluidization in the initiation and formation of Martian polar gullies. Geophysical Research Letters, 38, https://doi.org/10.1029/2011 GL049403
CHRISTENSEN, P.R. 1986. Regional dust deposits on Mars: physical properties, age, and history. Journal of Geophysical Research, 91, 3533-3545, https://doi.org/ 10.1029/JB091iB03p03533
COLEMAN, K.A., DIXON, J.C., HOWE, K.L., ROE, L.A. & CHEVRIER, V. 2009. Experimental simulation of Martian gully forms. Planetary and Space Science, 57, 711-716, https://doi.org/10.1016/j.pss.2008.11.002
CONWAY, S.J., LAMB, M.P., BALME, M.R., TOWNER, M.C. & MURRAY, J.B. 2011a. Enhanced runout and erosion by overland flow at low pressure and sub-freezing conditions: experiments and application to Mars. Icarus, 211, 443-457, https://doi.org/10.1016/j.icarus.2010. 08.026
CONWAY, S.J., BALME, M.R., MURRAY, J.B., TOWNER, M.C., OKUBO, C.H. & GRINDROD, P.M. 2011b. The indication of Martian gully formation processes by slope-area analysis. In: BALME, M.R., BARGERY, A.S., GALLAGHER, C.J. & GUPTA, S. (eds) Martian Geomorphology. Geological Society, London, Special Publications, 356, 171-201, https://doi.org/10.1144/SP356.10
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This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
Citations provided by BIP!popularityPopularity provided by BIP!
This indicator reflects the "current" impact/attention (the "hype") of an article in the research community at large, based on the underlying citation network.
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This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
Influence provided by BIP!impulseImpulse provided by BIP!
This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.
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Funded by
- University of Arkansas at Fayetteville United States
- Université Nantes
- Durham University United Kingdom
- Parthenope University of Naples Italy
- STFC Rutherford Appleton Laboratory United Kingdom
- University of Nantes France
- Planetary Science Institute United States
- Department of Earth Sciences University of Durham United Kingdom
- The Open University United Kingdom
Martian gullies were initially hypothesized to be carved by liquid water, due to their resemblance to gullies on Earth. Recent observations have highlighted significant sediment transport events occurring in Martian gullies at times and places where CO2 ice should be actively sublimating. Here we explore the role of CO2 sublimation in mobilizing sediment through laboratory simulation. In our previous experimental work, we reported the first observations of sediment slope movement triggered by the sublimation of CO2 frost. We used a Mars regolith simulant near the angle of repose. The current study extends our previous work by including two additional substrates, fine and coarse sand, and by testing slope angles down to 10°. We find that the Mars regolith simulant is active down to 17°, the fine sand is active only near the angle of repose and the coarse sand shows negligible movement. Using an analytical model, we show that under Martian gravity motion should be possible at even lower slope angles. We conclude that these mass-wasting processes could be involved in shaping Martian gullies at the present day and intriguingly the newly reported CO2-creep process could provide an alternative explanation for putative solifluction lobes on Mars.