Affiliation:
1. Malin Space Science Systems, Post Office Box 910148, San Diego, CA 92191–0148, USA.
Abstract
Relatively young landforms on Mars, seen in high-resolution images acquired by the Mars Global Surveyor Mars Orbiter Camera since March 1999, suggest the presence of sources of liquid water at shallow depths beneath the martian surface. Found at middle and high martian latitudes (particularly in the southern hemisphere), gullies within the walls of a very small number of impact craters, south polar pits, and two of the larger martian valleys display geomorphic features that can be explained by processes associated with groundwater seepage and surface runoff. The relative youth of the landforms is indicated by the superposition of the gullies on otherwise geologically young surfaces and by the absence of superimposed landforms or cross-cutting features, including impact craters, small polygons, and eolian dunes. The limited size and geographic distribution of the features argue for constrained source reservoirs.
Publisher
American Association for the Advancement of Science (AAAS)
Reference51 articles.
1. The debate over whether liquid water or some other liquid is responsible for fluid erosional landforms on Mars (including but not limited to the martian outflow channels and valley networks) is not specifically addressed in this work. Most geoscientists familiar with the martian landforms agree that water is the most likely candidate fluid (2); the only alternative is to speculate that some other completely unknown agent with properties essentially identical to those of water is or has been at work on Mars.
2. Baker V. R., et al., Geol. Soc. Am. Bull. 94, 1035 (1983).
3. Milton D. J., J. Geophys. Res. 78, 4037 (1973).
4. Climatic Change on Mars
5. Baker V. R., Milton D. J., Icarus 23, 27 (1974).
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