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Geomorphologic Evidence for Liquid Water

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Abstract

Besides Earth, Mars is the only planet with a record of resurfacing processes and environmental circumstances that indicate the past operation of a hydrologic cycle. However the present-day conditions on Mars are far apart of supporting liquid water on the surface. Although the large-scale morphology of the Martian channels and valleys show remarkable similarities with fluid-eroded features on Earth, there are major differences in their size, small-scale morphology, inner channel structure and source regions indicating that the erosion on Mars has its own characteristic genesis and evolution. The different landforms related to fluvial, glacial and periglacial activities, their relations with volcanism, and the chronology of water-related processes, are presented.

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Authors and Affiliations

  1. Université Paris-Sud, Equipe de Planétologie (UMR CRNS 8616), 91405, Orsay Cedex, France

    Philippe Masson & François Costard

  2. U.S. Geological Survey, MS-975, 345 Middlefield Road, Menlo Park, CA, 94025, USA

    Michael H. Carr

  3. Department of Geological Sciences, Arizona State University, Box 871404, Tempe, AZ, 85287-1404, USA

    Ronald Greeley

  4. DLR Institute of Space Sensor Technology and Planetary Exploration, Rutherfordstrasse 2, 12484, Berlin - Adlershof, Germany

    Ernst Hauber & Ralf Jaumann

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Masson, P., Carr, M.H., Costard, F. et al. Geomorphologic Evidence for Liquid Water. Space Science Reviews 96, 333–364 (2001). https://doi.org/10.1023/A:1011913809715

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