Ground ice on Mars: Inventory, distribution, and resulting landforms

Rossbacher, L. A.; Judson, Sheldon

doi:10.1016/0019-1035(81)90005-1

Cited by 147 publications

(95 citation statements)

References 40 publications

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“…Carr [1979] found that Martian megaregolith permeabilities as large as 3000 darcys were consistent with the discharge rates required for outflow channel formation. Ice likely fills the pores of near-surface materials to a depth ranging from 1 to 3 km at the equator and midlatitudes to a depth of approximately 3 to 8 km at the poles [Fanale, 1976, Rossbacher andJudson, 1981].…”

Section: Conceptual Modelmentioning

confidence: 99%

Magmatic intrusions and a hydrothermal origin for fluvial valleys on Mars

Gulick¹

1998

J. Geophys. Res.

196

203

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Abstract. Numerical models of Martian hydrothermal systems demonstrate that systems associated with magmatic intrusions greater than several hundred cubic kilometers can provide sufficient groundwater outflow to form the observed fluvial valleys, if subsurface permeability exceeds about 1.0 darcy. Groundwater outflow increases with increasing intrusion volume and subsurface permeability and is relatively insensitive to intrusion depth and subsurface porosity within the range considered here. Hydrothermally-derived fluids can melt through 1 to 2 km thick ice-rich permafrost layers in several thousand years. Hydrothermal systems thus provide a viable alternative to rainfall for providing surface water for valley formation. This mechanism can form fluvial valleys not only during the postulated early warm, wet climatic epoch, but also during more recent epochs when atmospheric conditions did not favor atmospheric cycling of water. The clustered distribution of the valley networks on a given geologic surface or terrain unit of Mars may also be more compatible with localized, hydrothermally-driven groundwater outflow than regional rainfall. Hydrothermal centers on Mars may have provided appropriate environments for the initiation of life or final oases for the long-term persistence of life.

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Section: Conceptual Modelmentioning

confidence: 99%

Magmatic intrusions and a hydrothermal origin for fluvial valleys on Mars

Gulick¹

1998

J. Geophys. Res.

196

203

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“…The martian cryosphere has been defined as that region of the crust where the temperature remains continuously below the freezing point of water (Fanale 1976, Rossbacher and Judson 1981, Kuzmin 1983. Assuming a solute-free freezing point of 273 K, this condition is satisfied at the surface at every latitude below the diurnal skin depth.…”

Section: Geothermal and Hydrologic Evolutionmentioning

confidence: 99%

“…Products of volcano-ice interactions appear to be widespread, especially at mid-latitudes (Allen 1979, Hodges and Moore 1979, Rossbacher and Judson 1981, Mouginis-Mark 1985, Squyres et al 1987, Christiansen 1989, Chapman 1994, Garvin et al 2000. Other terrains appear to have been formed by ice-assisted mass wasting, ablation, and other types of periglacial activity (Carr and Schaber 1977, Howard 198 1, Lucchitta 1981, Squyres and Carr 1986.…”

Section: The Geologic Evidence For and Against Glacial Flowmentioning

confidence: 99%

The State and Future of Mars Polar Science and Exploration

Clifford

2000

Icarus

110

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20, 1999; revised October 25, 1999 As the planet's principal cold traps, the martian polar regions have accumulated extensive mantles of ice and dust that cover individual areas of -lo6 km2 and total as much as 3-4 km thick. From the scarcity of superposed craters on their surface, these layered deposits are thought to be comparatively young-preserving a record of the seasonal and climatic cycling of atmospheric COz, H20, and dust over the past NIO~-IO~ years..For this reason, the martian polar deposits may serve as a Rosetta Stone for understanding the geologic and climatic history of the planet--documenting variations in insolation (due to quasiperiodic oscillations in the planet's obliquity and orbital elements), volatile mass balance, atmospheric composition, dust storm activity, volcanic eruptions, large impacts, catastrophic floods, solar luminosity, supernovae, and perhaps even a record of microbial life. Beyond their scientific value, the polar regions may soon prove important for another reason-providing a valuable and accessible reservoir of water to support the long-term human exploration of Mars. In this paper we assess the current state of Mars polar research, identify the key questions that motivate the exploration of the polar regions, discuss the extent to which current missions will address these questions, and speculate about what additional capabilities and investigations may be required to address the issues that remain outstanding.

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“…On comprend alors toute l'efficacité de la cryokarstie quand on sait que, pour la Lena, le recul des versants parallèlement à eux-mêmes peut atteindre, en certains cas, une valeur proche de 25 m/an 1983). La richesse en matériaux volatils du pergélisol martien n'est guère quantifiable actuellement; les valeurs absolues théoriques ont été estimées supérieures à 40 % (Rossbacher and Judson, 1981). Le volume minimal des terrains chaotiques et des vallées associées a été estimé à 3,26 millions de km 3 .…”

Section: Les Valléesunclassified

Vallées de débâcle et processus cryokarstiques sur Mars et en Sibérie

Costard¹

2007

gpq

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RÉSUMÉLe climat froid et sec de la planète Mars implique le maintien d'un pergélisol. À Yakutsk (Sibérie), l'épaisseur maximale du pergélisol est de 1,5 km. Une analyse comparative entre les vallées de débâcle en Sibérie et celles de la planète Mars est proposée. Elle fait appel au processus d'érosion thermique produit par le contact de l'eau liquide avec le pergélisol. La fonte des glaces de ségrégation sous la vallée implique la formation d'un talik. Celui-ci facilite la prise en charge des sédiments et l'enfoncement de la vallée. En Sibérie, le sapement le long des berges par érosion thermique provoque un rapide recul des versants qui expliquerait la largeur excessive des vallées de débâcle sur Mars. Avec le climat froid de la planète Mars et de la Sibérie, le pergélisol, empêche l'infiltration de l'eau tout en facilitant l'étalement des sédiments à l'embouchure des vallées. La présence de couches massives de glace dans le sous-sol et leurs fontes préférentielles contribue au développement d'un cryokarst comme celui des vallées d'alas en Yakoutie. Une comparaison est proposée entre le cryokarst de la Yakoutie et certaines dépressions fermées sur Mars.

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Ground ice on Mars: Inventory, distribution, and resulting landforms

Cited by 147 publications

References 40 publications

Magmatic intrusions and a hydrothermal origin for fluvial valleys on Mars

Magmatic intrusions and a hydrothermal origin for fluvial valleys on Mars

The State and Future of Mars Polar Science and Exploration

Vallées de débâcle et processus cryokarstiques sur Mars et en Sibérie

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