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Crater Lakes on Mars: Development of Quantitative Thermal and Geomorphic ModelsImpact craters on Mars have served as catchments for channel-eroding surface fluids, and hundreds of examples of candidate paleolakes are documented [1,2] (see Figure 1). Because these features show similarity to terrestrial shorelines, wave action has been hypothesized as the geomorphic agent responsible for the generation of these features [3]. Recent efforts have examined the potential for shoreline formation by wind-driven waves, in order to turn an important but controversial idea into a quantitative, falsifiable hypothesis. These studies have concluded that significant wave-action shorelines are unlikely to have formed commonly within craters on Mars, barring Earth-like weather for approx.1000 years [4,5,6].
Document ID
20050201828
Acquisition Source
Headquarters
Document Type
Conference Paper
Authors
Barnhart, C. J. (California Univ. Santa Cruz, CA, United States)
Tulaczyk, S. (California Univ. Santa Cruz, CA, United States)
Asphaug, E. (California Univ. Santa Cruz, CA, United States)
Kraal, E. R. (California Univ. Santa Cruz, CA, United States)
Moore, J. (NASA Ames Research Center Moffett Field, 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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