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    An atmospheric blast/thermal model for the formation of high-latitude pedestal craters

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    Author
    Wrobel, Kelly
    Schultz, Peter
    Crawford, David
    Issue Date
    2006-01-01
    Keywords
    Impact vaporization
    Mars pedestal craters
    Martian atmosphere
    Mars volatiles
    
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    Citation
    Wrobel, K., Schultz, P., & Crawford, D. (2006). An atmospheric blast/thermal model for the formation of high‐latitude pedestal craters. Meteoritics & Planetary Science, 41(10), 1539-1550.
    Publisher
    The Meteoritical Society
    Journal
    Meteoritics & Planetary Science
    Description
    From the proceedings of the Workshop on the Role of Volatiles and Atmospheres on Martian Impact Craters held on July 11-14, 2005, at the Johns Hopkins University Applied Physics Laboratory.
    URI
    http://hdl.handle.net/10150/656197
    DOI
    10.1111/j.1945-5100.2006.tb00434.x
    Additional Links
    https://meteoritical.org/
    Abstract
    Although tenuous, the atmosphere of Mars affects the evolution of impact-generated vapor. Early-time vapor from a vertical impact expands symmetrically, directly transferring a small percentage of the initial kinetic energy of impact to the atmosphere. This energy, in turn, induces a hemispherical shock wave that propagates outward as an intense airblast (due to high-speed expansion of vapor) followed by a thermal pulse of extreme atmospheric temperatures (from thermal energy of expansion). This study models the atmospheric response to such early-time energy coupling using the CTH hydrocode written at Sandia National Laboratories. Results show that the surface surrounding a 10 km diameter crater (6 km "apparent" diameter) on Mars will be subjected to intense winds (~200 m/s) and extreme atmospheric temperatures. These elevated temperatures are sufficient to melt subsurface volatiles at a depth of several centimeters for an ice-rich substrate. Ensuing surface signatures extend to distal locations (~4 apparent crater diameters for a case of 0.1% energy coupling) and include striations, thermally armored surfaces, and/or ejecta pedestals--all of which are exhibited surrounding the freshest high-latitude craters on Mars. The combined effects of the atmospheric blast and thermal pulse, resulting in the generation of a crater-centered erosion-resistant armored surface, thus provide a new, very plausible formation model for high-latitude Martian pedestal craters.
    Type
    Proceedings
    text
    Language
    en
    ISSN
    1945-5100
    ae974a485f413a2113503eed53cd6c53
    10.1111/j.1945-5100.2006.tb00434.x
    Scopus Count
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    Meteoritics & Planetary Science, Volume 41, Number 10 (2006)

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