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NARROW
GeoRef Subject
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all geography including DSDP/ODP Sites and Legs
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Arctic region
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Greenland (1)
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Asia
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Himalayas (1)
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Indian Peninsula
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minerals
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silicates
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sheet silicates (1)
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Primary terms
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Arctic region
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Greenland (1)
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Asia
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Himalayas (1)
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Indian Peninsula
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India (1)
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Jammu and Kashmir
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Ladakh (1)
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Canada
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Eastern Canada
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Nirgal Vallis
Figure 2. Data for gullies at Dao Vallis, Nirgal Vallis, and Hale Crater. A...
Figure 2. Channels on floors of Martian valley networks, using THEMIS (see ...
Role of aquicludes in formation of Martian gullies
Figure 1. Examples of gullies in each of three study regions. Each scale ba...
HiRISE imaging of impact megabreccia and sub-meter aqueous strata in Holden Crater, Mars
Interior channels in Martian valley networks: Discharge and runoff production
Unique chronostratigraphic marker in depositional fan stratigraphy on Mars: Evidence for ca. 1.25 Ma gully activity and surficial meltwater origin
Geomorphologic observations and physical hypothesis on Martian gullies
Substrate controls on valley formation by groundwater on Earth and Mars
Abstract We conducted comparative morphological analysis of gullies within two high-latitude Martian craters (Domoni and Maricourt) in the northern hemisphere of Mars with (1) the debris-flow gully systems in the Ladakh Himalaya and (2) Istok Crater in the southern mid-latitudes of Mars where water-bearing debris-flow deposits have been previously reported. Our findings suggest that the debris-flow landforms preserved on gully and alluvial fans in the Ladakh Himalaya are potential analogues for the deposits preserved over the equator-facing slopes of Domoni and Maricourt Craters. Further, we found that the morphological attributes of channels and deposits (including overlapping terminal lobes, levées, tongue-shaped/lobate deposits and broad/small depositional deposits) within both the study craters and Istok Crater are similar. As a result, the studied craters emerge as additional sites in which possible evidence of water-bearing debris-flows are preserved on Mars. By comparison to our Earth analogue, we further propose that episodic melting of snow accumulated within the sheltered alcoves is the most likely source of water for the formation of such gullies. Taken together, our findings suggest that debris-flow may not be a rare process in gully formation on Mars and evidence may be preserved in other unexplored areas.
Martian gullies: a comprehensive review of observations, mechanisms and insights from Earth analogues
Abstract Upon their discovery in 2000, Martian gullies were hailed as the first proof of recent (i.e. less than a few million years) flowing liquid water on the surface of a dry desert planet. Many processes have been proposed to have formed Martian gullies, ranging from liquid-water seepage from aquifers, melting of snow, ice and frost, to dry granular flows, potentially lubricated by CO 2 . Terrestrial analogues have played a pivotal role in the conception and validation of gully-formation mechanisms. Comparison with the terrestrial landscape argues for gully formation by liquid-water debris flows originating from surface melting. However, limited knowledge of sediment transport by sublimation is a critical factor in impeding progress on the CO 2 -sublimation hypothesis. We propose avenues towards resolving the debate: (a) laboratory simulations targeting variables that can be measured from orbit; (b) applications of landscape-evolution models; (c) incorporation of the concept of sediment connectivity; (d) using 3D fluid-dynamic models to link deposit morphology and flow rheology; and (e) a more intense exchange of techniques between terrestrial and planetary geomorphology, including quantitative and temporal approaches. Finally, we emphasize that the present may not accurately represent the past and that Martian gullies likely formed by a combination of processes.