Other
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....9716183s&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. E10, p. 16,183-16,248.
Other
107
Atmospheric Effects, Cratering, Ejecta, Meteorite Craters, Planetary Craters, Venus Atmosphere, Venus Surface, Energy Transfer, Gravitational Effects, Magellan Project (Nasa)
Scientific paper
Surface signatures of energy partitioning are used as a framework for testing extrapolations from laboratory experiments and other planetary settings to assess the effects of both gravity and an atmosphere on impact crater formation on Venus. The dense lower atmosphere of Venus is found to assume the role of a low-density target for bodies smaller than about 4 km in diameter. Air blasts created by cratering in the atmosphere produce distinctive surface signatures that allow the derivation of an independent assessment of impactor energy at the limit of break up. Dynamic pressures during entry of larger bodies will exceed their strength limit but may not prevent penetration of the atmosphere due to aerodynamic reshaping that minimizes the drag coefficient. This process may account for the formation of unusually small craters (1-3 km). The dense atmosphere of Venus preserves signatures of early time cratering processes on the surface that are typically lost on atmosphere-free surfaces.
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