TY - JOUR
T1 - A review of Martian impact crater ejecta structures and their implications for target properties
AU - Barlow, Nadine G.
PY - 2005
Y1 - 2005
N2 - Most fresh Martian impact craters are surrounded by layered ("fl uidized") 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 co tribution, 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.
AB - Most fresh Martian impact craters are surrounded by layered ("fl uidized") 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 co tribution, 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.
KW - Ejecta blanket
KW - Mars craters
KW - Subsurface volatiles
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U2 - 10.1130/0-8137-2384-1.433
DO - 10.1130/0-8137-2384-1.433
M3 - Article
AN - SCOPUS:73949138997
SN - 0072-1077
VL - 384
SP - 433
EP - 442
JO - Special Paper of the Geological Society of America
JF - Special Paper of the Geological Society of America
ER -