Two Different Supply Styles of Crater Outflow Materials on Venus Inferred from Numerical Simulations over DEMs

Initiation of Run-Out Flows on Venus by Oblique Impacts

“…In fact, the high atmospheric pressure of Venus allows condensation of impact vapor at high temperature, which makes it more likely for a liquid phase to be dominant rather than a solid phase. It also should be noted, however, that some of the low viscosity values may not be necessary to account for the flow patterns if the mass discharge rate of the flows are very large (Miyamoto and Sasaki 2000).…”

Impact ejecta emplacement on terrestrial planets

“…This attests to an initial emplacement mode that was highly energetic. Three dimensional numerical simulations of the outflows separated them into two types: "catastrophic" outflows originating at or near the rim, with outflow rates of 10 10 m 3 /s lasting less than 100 s, and "gentle" outflows originating in the ejecta, with outflow rates of 10 4 m 3 /s lasting more than 10 5 s (Miyamoto and Sasaki, 2000). The emplacement of the catastrophic outflows was attributed directly to the cratering process, while that of the gentle outflows was attributed to secondary segregation and drainage of melt materials from within previously emplaced ejecta.…”

Impact Melting

“…Asimow and Wood (1992) recognized erosive, channel-forming outflows of what was probably impact melt that may consist of a mix of solid and melt. Threedimensional numerical simulations of the outflows separated them into two types: 'catastrophic' outflows originating at or near the rim, with outflow rates of 10 10 m 3 s −1 lasting less than 100 s, and 'gentle' outflows originating in the ejecta, with outflow rates of 10 4 m 3 s −1 lasting more than 10 5 s (Miyamoto and Sasaki, 2000). The emplacements of the catastrophic outflows were attributed directly to the cratering process, while the gentle outflows were attributed to secondary segregation and drainage of melt materials from within previously emplaced ejecta.…”