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Distribution and Orientation of Alluvial Fans in Martian CratersWe present the results of the complete survey of Martian alluvial fans from 0-30 S, initiated by Moore and Howard. Nineteen impact craters contain alluvial fans. They are regionally grouped into three distinct areas. We present our initial results regarding their distribution and orientation in order to understand what controls their formation. Since alluvial fans are formed by water transport of sediment, these features record wetter episodes of Martian climate. In addition, their enigmatic distribution (in regional groups and in some craters, but not similar adjacent ones) needs to be understood, to see how regional geology, topographic characteristics, and/or climate influence their formation and distribution.
Document ID
20050201856
Acquisition Source
Headquarters
Document Type
Conference Paper
Authors
Kraal, E. R. (California Univ. Santa Cruz, CA, United States)
Moore, J. M. (NASA Ames Research Center Moffett Field, CA, United States)
Howard, A. D. (Virginia Univ. Charlottesville, VA, United States)
Asphaug, E. I. (California Univ. Santa Cruz, CA, United States)
Date Acquired
September 7, 2013
Publication Date
January 1, 2005
Publication Information
Publication: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters
Subject Category
Lunar And Planetary Science And Exploration
Distribution Limits
Public
Copyright
Public Use Permitted.

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IDRelationTitle20050201815Collected WorksWorkshop on The Role of Volatile and Atmospheres on Martian Impact Craters
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