Other
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27.1481y&link_type=abstract
Lunar and Planetary Science, volume 27, page 1481
Other
Fractality, Outflows: Impact Crater, Venus
Scientific paper
402 out of 932 Venusian impact craters have outflows (Chadwick and Schaber, 1993a, b; Schaber and Chadwick, 1993) originating from inside or under the ejecta blankets. They differ from the ejecta blanket by their length, brightness, nonradiality, morphology, and/or sinuous planform (Asimow and Wood, 1992) and are too long to be caused by ballistic processes (Chadwick and Schaber, 1993b). These low viscosity flows have traveled up to hundreds kilometers, possibly due to large amounts of entrained hot gases and impact melt. In places they surmount structures of considerable height but their relation to the topography varies (Schaber et al., 1992). A few of them are erosional, with streamlined islands and a large drainage areas close to the crater, but most are depositional. Some deposits are structureless and less organized, while others have channels with margins or levees (Asimow and Wood, 1992). Outflow deposits are fairly thin, and their directions may have been controlled by the local topography (Schaber et al., 1992). The fluid identity and emplacement mechanisms are not understood. Outflows have various relations to ejecta deposition.
Kauhanen K.
Raitala Jouko
You Jiangong
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