Journal of Geophysical Research (Planets), Volume 108, Issue E5, pp. 5-1, CiteID 5039, DOI 10.1029/2002

Aqueous flows carved the outflow channels on Mars

Author: Coleman, Neil M.

Abstract

The role of water in carving the Martian outflow channels has recently been challenged by the hypothesis known as ``White Mars.'' This hypothesis claims that the channels were cut by CO2 gas-supported debris flows that also resurfaced the northern plains. However, proposed analogs of ``cryoclastic'' flows are either inappropriate (i.e., submarine density flows) or are primarily depositional rather than erosional (i.e., pyroclastic flows). Subaerial mass movements on Earth do not carve long deep channels like those on Mars. I review runout efficiencies for mass movements on Earth and Mars. The efficiencies required for ``cryoclastic'' flows to resurface the northern plains of Mars are so large that they appear unattainable. White Mars seeks to resolve carbonate and floodwater ``paradoxes'' that probably do not exist. It is also doubtful whether reservoirs of CO2 could persist over geologic time in the crust. Overall, the CO2 hypothesis fails key tests and should be abandoned as a means to carve outflow channels. I present a new interpretation of the fluid source that created Aromatum Chaos and Ravi Vallis. Water, not liquid or gaseous CO2, was the causative fluid, and the source was an ice-covered impoundment in ancestral Ganges Chasma. At that time the canyon had no eastern outlet, and groundwater flowed northward to discharge at Aromatum Chaos and Shalbatana Vallis. The presence of ice-covered water bodies can help to calibrate models of volcanic-hydrologic climaxes during Hesperian time. The outflow channels, like the spectacular landforms of the Channeled Scabland, are monuments to the erosive power of catastrophic aqueous floods.

And of course these others among many:

D.M. Nelson, R. Greeley “XANTHE TERRA OUTFLOW CHANNEL GEOLOGY AT THE MARS PATHFINDER LANDING SITE” Lunar and Planetary Science XXIX 1158.pdf
http://mars.jpl.nasa.gov/MPF/science/lpsc98/1158.pdf

“Summary. Geologic mapping of southern Chryse Planitia and the Xanthe Terra outflow channels has revealed a sequence of fluvial events which contributed sediment to the Mars Pathfinder landing site (MPLS). Three major outflow episodes are recognized: (1) broad sheetwash across Xanthe Terra during the Early Hesperian period, (2) Early to Late Hesperian channel formation of Shalbatana, Ravi, Simud, Tiu, and Ares Valles, and (3) subsequent flooding which deepened the channels to their current morphologies throughout the Late Hesperian. Materials from the most recent flooding, from Simud and Tiu Valles, and (to a lesser extent) materials from Ares Vallis, contributed the greatest amount of sediment to MPLS.”

Bradley J. Thomson and James W. Head III “Utopia Basin, Mars: Characterization of topography and morphology and assessment of the origin and evolution of basin internal structure” JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 106, NO. 0, PAGES 1–22, MONTH 2001 available online at
http://www.planetary.brown.edu/planetary/documents/2396.pdf

“8.4. Glacial Features
Another possible explanation of the circumferential features is
that they are related to morainal/ice-margin features. A glacial
explanation has been advanced for the formation of thumbprint
terrain [Lucchitta, 1981; Rossbacher, 1985; Lucchitta et al., 1987;
Scott and Underwood, 1991; Scott et al., 1992; Kargel and Strom,
1992; Kargel et al., 1995]. As shown in Figure 10, there are areas of
thumbprint terrain that are located in the middle of the zone of
circumferential features in southern Utopia. On the basis of the
morphology and distribution of thumbprint terrain and other structures,
several workers have suggested the former presence of large
ice sheets in the northern hemisphere of Mars [Lucchitta et al.,
1986; Chapman, 1994; Kargel et al., 1995]. The lack of associated
glacial flow features such as drumlins in the northern plains seems
inconsistent with widespread glacial activity. Drumlins are streamlined
mounds of glacial till that have elongated teardrop shapes in
plan view [Benn and Evans, 1998]. The absence of drumlins does
not rule out a glacial explanation, for a glacial body in the northern
hemisphere may have been cold-based for much of its evolution
[e.g., Kargel et al., 1995]. However, the lack of drumlins highlights
the general lack of features related to mass ice movement and scour
in the interior of the Northern Plains. In addition, because ice
experiences a drop in plasticity with decreasing temperature [Glen,
1955; Goldsby et al., 2001], the current temperature regime on Mars
would tend to inhibit glacial flow. This does not exclude the possibility of glacial activity at periods of high obliquity or more
temperate paleoclimatic conditions but highlights the need for a
greater understanding of ice deformation mechanisms [Goldsby et
al., 2001] under possible Martian paleoclimates before the viability
of a glacial explanation can be verified.”

“Carr (1996) suggested that ground water flowed from the Tharsis uplands into the deep canyons of Valles Marineris before debouching onto Chryse Planitia in the northern plains. Such a flow may have persisted for billions of years, and is generally inferred to have maintained deep lakes beneath which lacustrine sediments accumulated. Remnants of these Hesperian Age lake deposits survive today as conspicuous layered
strata in Central Valles Marineris. Just published MOLA data (Smith, et al, 1999) confirm in detail this topographic trend and, most importantly, prove that deep, permanent lakes did indeed exist, especially in Central and Western Valles Marineris. Because the canyons in the Valles Marineris are deeper than the probable ground water table at that period, large portions of the canyons would have filled with water and formed ice-covered lakes.”
http://web99.arc.nasa.gov/~vgulick/MSLS99_Wkshp/Murray_Paleolakes_VM_abs.pdf

John A. Grant “DRAINAGE EVOLUTION IN MARGARITIFER SINUS, MARS” Paper No. 132-0 GSA Annual Meeting, November 5-8, 2001 Boston, Massachusetts

“Geologic mapping in Margaritifer Sinus, Mars, defines a complex history of water transport, storage, and release that began in the late Noachian and persisted into at least the mid-Hesperian. Collection, transport, and discharge of the water from widely dispersed surfaces were accomplished by systems of differing character flanking opposite sides of the Chryse Trough. Drainage on the western side of the trough was accommodated by the segmented Uzboi-Ladon-Margaritifer mesoscale outflow system that heads in Argyre basin, drains approximately 9% of the Martian surface, and alternately incises and fills as it crosses ancient multi-ringed impact basins.”
http://gsa.confex.com/gsa/2001AM/finalprogram/abstract_27669.htm

Parker et al., [2000], LPSC XXXI, 2033.pdf

“Catastrophic flooding out of Argyre: Uzboi Valles is a relatively large, Noachian outflow channel that cuts the northern rim of Argyre (Nereidum Montes) and drained northward toward Holden Crater, into Holden Basin [7]. Without good topography, however, Uzboi Valles is somewhat confusing. With both ends obliterated by large impact craters and the channel floor exhibiting few streamlined forms, it isn’t even obvious which way the channel flowed. However, even the gridded MOLA topography clearly shows Uzboi probably linked the Argyre interior with Holden Basin and Ladon Valles prior to formation of the large craters (Fig. 1). Next in the system is Holden Basin [7], into which Uzboi Vallis flow continued prior to formation of Holden Crater [2]. The northeast rim of Holden Basin is “gone” even though this basin superposes Ladon Basin. Instead, a broad “ramp” was identified in Viking Orbiter stereo pairs [2]. Ladon and Arda Valles converge on this ramp and drain into the interior of Ladon Basin. Parker [2] inferred that the rim of Holden Basin failed catastrophically during flooding from Argyre to produce this ramp, which drained a temporary lake that had formed in Holden Basin. Continued flooding from Uzboi Vallis favored Ladon Valles’ course, so Arda Valles was quickly abandoned. Channel morphology disappears just inside the inner rim of Ladon Basin, but resumes on the basin’s northeast side, at Margaritifer Valles [8].”
http://www.lpi.usra.edu/meetings/lpsc2000/pdf/2033.pdf