Computer Science
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27.1143s&link_type=abstract
Lunar and Planetary Science, volume 27, page 1143
Computer Science
Atmospheric Interaction, Craters, Impacts, Pressure, Venus
Scientific paper
The question of atmospheric effects in crater formation was addressed by Schmidt and Hassig (1995) and Schmidt et al.(1995) using numerical simulation. Presentation of these earlier results are somewhat obscured by scaling models that relate spacial and temporial variables to crater size and time of formation. The results shown here are unscaled and shown in prototype dimensions. The original 10-km impactor calculation performed by Hassig (1991) used a numerical artifact to create a "transparent" target allowing the impactor to pass through the surface. Hence, the calculated aerodynamic effects were due only to the entry shock wave. There was concern that vaporization might provide an additional contribution to the flow field. Likewise, a compliant cratering target would cause some vaporization while at the same time absorbing a lot of the kinetic energy in the form of coupling to the ground leading to crater formation. To evaluate the effects of these various boundary conditions, two additional calculations were run. One had a rigid surface, causing the impactor to arrest, vaporize and rebound upon contact. The second used a coarsely-zoned quartz-like material to allow crater formation to take place. In the early time, close in, there were significant differences. However at the range of expected final crater radius, the profiles all more or less coalesce.
Hassig P. J.
Housen Kevin R.
Schmidt Mirek R.
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