Computer Science – Sound
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27...61b&link_type=abstract
Lunar and Planetary Science, volume 27, page 61
Computer Science
Sound
Ames Vertical Gun Range, Ejecta Flow Lobes, Impacts, Mars: Atmosphere, Rings: Vortex
Scientific paper
Distal flow lobes around craters on planets with atmospheres may result from the formation of waves in a ring vortex created by flow separation at the top edge of an advancing impact ejecta curtain. The number of waves in a smoke ring is controlled by two factors: 1.) the ratio of the radius of the ring vortex (Rv) to its core radius (a); and, 2.) the intensity of the flow in the ring vortex core. At laboratory scales, the number of ejecta flows from ejecta-driven ring vortices varies with these factors in the same fashion as waves of a smoke ring. Theoretical and laboratory studies indicate that the number of flow lobes created during an impact varies with the crater radius (R) to the three-fourths power (i.e. R3/4). Lobe counts on Mars and Venus confirm this correlation for those craters whose radii do not exceed the scale height of the atmosphere and where the flow in the ring vortex does not exceed the ambient speed of sound. The formation of flow lobes by ring vortices created by the motion of the ejecta curtain, are consistent, therefore, with observation at planetary scales. Variations in the number of lobes on Mars could indicate variations in target lithologies, presence of volatiles or changes in atmospheric conditions. Further work will establish which of these contributing factors most affects the number of distal lobes created during an impact.
Barnouin-Jha Olivier Serge
Schultz Peter H.
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