Physics
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt.........2b&link_type=abstract
Thesis (PHD). BROWN UNIVERSITY , Source DAI-B 59/04, p. 1548, Oct 1998, 288 pages.
Physics
Scientific paper
Many mechanisms have been proposed to explain the origin of fluidized ejecta morphologies observed at craters formed by an asteroid or comet colliding with a planetary surface. The predominant mechanisms include: the incorporation of water or volatiles into a subsequently fluidized ejecta flow resembling a mudslide; the incorporation of air and volatiles into a debris cloud of primary and secondary ejecta that slides along the target surface; the formation of an ejecta ''sturzstrom' following the gravitational collapse of an ejecta curtain that has been decelerated and steepened by impinging atmosphere; and, the formation of strong atmospheric winds generated by an advancing ejecta curtain that entrain and deposit ejecta. Laboratory experiments show that this last mechanism produces fluidized ejecta facies with contiguous ramparts and lobate flows that are remarkably similar to features seen on Mars, Venus and the Earth. In order to quantitatively assess the importance of such winds at planetary scales, this thesis combines a variety of analytical, numerical and empirical techniques to investigate the interactions between an advancing ejecta curtain and an atmosphere. The physical models developed describe the entrainment capacity and initial transport of ejecta by these winds, as well as some of the factors controlling ejecta deposition. The ultimate objective of this study is to model most aspects of ejecta entrainment, transport and deposition. In combination with observations of fluidized ejecta facies, such models should provide new insight into the target and atmospheric conditions present during crater formation. Such information may improve our understanding of past climatic and surface conditions on planets such as Mars.
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