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A review of Martian impact crater ejecta structures and their implications for target properties

By
Nadine G. Barlow
Nadine G. Barlow
Department of Physics and Astronomy, Northern Arizona University, Flagstaff, Arizona 86011-6010, USA
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Published:
January 01, 2005

Most fresh Martian impact craters are surrounded by layered (“fluidized”) ejecta which were emplaced as flow deposits. Observational data, laboratory experiments, and numerical modeling strongly suggest that particle size, particle density, atmospheric density and pressure, and the presence of subsurface volatiles all contribute to the features observed in these craters and their ejecta blankets. In this contribution, we review the evidence that both subsurface volatiles and the thin Martian atmosphere contribute to the morphologic, morphometric, and thermophysical characteristics of Martian impact craters and their ejecta deposits.

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Contents

GSA Special Papers

Large Meteorite Impacts III

Thomas Kenkmann
Thomas Kenkmann
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Friedrich Hörz
Friedrich Hörz
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Alex Deutsch
Alex Deutsch
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Geological Society of America
Volume
384
ISBN print:
9780813723846
Publication date:
January 01, 2005

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