Morphometric measurements of martian valley networks from Mars Orbiter Laser Altimeter (MOLA) data

Williams, R. M. E.; Phillips, R. J.

doi:10.1029/2000je001409

Cited by 99 publications

(76 citation statements)

References 52 publications

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“…The flat floor of this cross section is much wider than any ephemeral waterfall that flows over the headscarp, such that abrasion, plucking, and spray resulting from surface flooding are ineffective weathering and erosional agents for most of the width of the headscarp. (For many martian examples, the trapezoidal cross section may be a secondary feature resulting from mass wasting and aeolian infilling of ancient valleys rather than the primary morphology described here (Williams and Phillips, 2001). ) Identifying dominant seepage erosion is straightforward, as the downstream channel dimensions and transported particle sizes should be consistent with measured spring discharges rather than much larger surface floods generated by precipitation.…”

Section: Characteristic Featuresmentioning

confidence: 99%

“…These alternative hypotheses should be considered when interpreting theaterheaded valleys, which should not be attributed by default to groundwater sapping on the basis of planform morphology alone. Secondary infilling of the valley after flow ceased should also be considered when attempting to explain the development of flat valley floors on Mars (Williams and Phillips, 2001).…”

Section: Implications For Interpretation Of Marsmentioning

confidence: 99%

“…Valley cross sections are locally V-shaped (particularly on steeper regional slopes, e.g., Fig. 1) but more commonly are trapezoidal, with a flat floor (Baker and Partridge, 1986;Goldspiel et al, 1993;Williams and Phillips, 2001).…”

Section: Introductionmentioning

confidence: 99%

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Origin and development of theater-headed valleys in the Atacama Desert, northern Chile: Morphological analogs to martian valley networks

Irwin

Tooth

Craddock

et al. 2014

Icarus

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a b s t r a c tUnderstanding planetary landforms, including the theater-headed valleys (box canyons) of Mars, usually depends on interpreting geological processes from remote-sensing data without ground-based corroboration. Here we investigate the origin and development of two Mars-analog theater-headed valleys in the hyperarid Atacama Desert of northern Chile. Previous workers attributed these valleys to groundwater sapping based on remote imaging, topography, and publications on the local geology. We evaluate groundwater sapping and alternative hypotheses using field observations of characteristic features, strength measurements of strata exposed in headscarps, and estimates of ephemeral flood discharges within the valleys. The headscarps lack evidence of recent or active seepage weathering, such as spring discharge, salt weathering, alcoves, or vegetation. Their welded tuff caprocks have compressive strengths multiple times those of the underlying epiclastic strata. Flood discharge estimates of cubic meters to tens of cubic meters per second, derived using the Manning equation, are consistent with the size of transported clasts and show that the ephemeral streams are geomorphically effective, even in the modern hyperarid climate. We interpret that headscarp retreat in the Quebrada de Quisma is due to ephemeral flood erosion of weak Miocene epiclastic strata beneath a strong welded tuff, with erosion of the tuff facilitated by vertical jointing. The Quebrada de Humayani headscarp is interpreted as the scar of a giant landslide, maintained against substantial later degradation by similar strong-over-weak stratigraphy. This work suggests that theater-headed valleys on Earth and Mars should not be attributed by default to groundwater sapping, as other processes with lithologic and structural influences can form theater headscarps.Published by Elsevier Inc.

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Section: Characteristic Featuresmentioning

confidence: 99%

Section: Implications For Interpretation Of Marsmentioning

confidence: 99%

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Origin and development of theater-headed valleys in the Atacama Desert, northern Chile: Morphological analogs to martian valley networks

Irwin

Tooth

Craddock

et al. 2014

Icarus

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“…Knowledge of the topography permits extension of such analyses by using additional quantitative criteria. Longitudinal stream profiles, locations of channels relative to surface topography, and transverse cross sections of valleys (12,13) may now be used to constrain the genesis and evolution of Martian valleys.…”

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confidence: 99%

Drainage basins and channel incision on Mars

Aharonson

Zuber

Rothman

et al. 2002

Proc. Natl. Acad. Sci. U.S.A.

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Measurements acquired by the Mars Orbiter Laser Altimeter on board the Mars Global Surveyor indicate that large drainage systems on Mars have geomorphic characteristics inconsistent with prolonged erosion by surface runoff. We find the topography has not evolved to an expected equilibrium terrain form, even in areas where runoff incision has been previously interpreted. By analogy with terrestrial examples, groundwater sapping may have played an important role in the incision. Longitudinally flat floor segments may provide a direct indication of lithologic layers in the bedrock, altering subsurface hydrology. However, it is unlikely that floor levels are entirely due to inherited structures due to their planar cross-cutting relations. These conclusions are based on previously unavailable observations, including extensive piece-wise linear longitudinal profiles, frequent knickpoints, hanging valleys, and small basin concavity exponents.

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“…Upstream they either become shallower and more V-shaped or they retain their downstream cross section until they terminate in a broad alcove. The more prominent valleys are typically incised into the surface to a depth of 50-300 m [9] and the depth of incision may remain almost constant for large distances. Typically, the more prominent valleys are outlined by steep walls with an abrupt scarp at the edge of the upland surface.…”

Section: Valley Networkmentioning

confidence: 99%

The fluvial history of Mars

Carr

2012

Phil. Trans. R. Soc. A.

103

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River channels and valleys have been observed on several planetary bodies in addition to the Earth. Long sinuous valleys on Venus, our Moon and Jupiter's moon Io are clearly formed by lava, and branching valleys on Saturn's moon Titan may be forming today by rivers of methane. But by far the most dissected body in our Solar System apart from the Earth is Mars. Branching valleys that in plan resemble terrestrial river valleys are common throughout the most ancient landscapes preserved on the planet. Accompanying the valleys are the remains of other indicators of erosion and deposition, such as deltas, alluvial fans and lake beds. There is little reason to doubt that water was the erosive agent and that early in Mars' history, climatic conditions were very different from the present cold conditions and such that, at least episodically, water could flow across the surface. In addition to the branching valley networks, there are large flood features, termed outflow channels. These are similar to, but dwarf, the largest terrestrial flood channels. The consensus is that these channels were also cut by water although there are other possibilities. The outflow channels mostly postdate the valley networks, although most are still very ancient. They appear to have formed at a time when surface conditions were similar to those that prevail today. There is evidence that glacial activity has modified some of the water-worn valleys, particularly in the 30-50 • latitude belts, and ice may also be implicated in the formation of geologically recent, seemingly water-worn gullies on steep slopes. Mars also has had a long volcanic history, and long, sinuous lava channels similar to those on the Moon and Venus are common on and around the large volcanoes. These will not, however, be discussed further; the emphasis here is on the effects of running water on the evolution of the surface.

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Morphometric measurements of martian valley networks from Mars Orbiter Laser Altimeter (MOLA) data

Cited by 99 publications

References 52 publications

Origin and development of theater-headed valleys in the Atacama Desert, northern Chile: Morphological analogs to martian valley networks

Origin and development of theater-headed valleys in the Atacama Desert, northern Chile: Morphological analogs to martian valley networks

Drainage basins and channel incision on Mars

The fluvial history of Mars

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