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- ( - , - 840 , - 30 )

cm.

The rims of two simple impact craters, Wolfe Creek, Australia, and Meteor Crater, AZ, USA, were examined. New methods of analysis were devised to display structural features that may be indicative of oblique impacts. Data from the two craters are compared.
Although the majority of craters are formed by oblique impacts, crater shapes remain circular for impact angles >30 and thus normally do not give any implications for the direction of impact. However, the ejecta blanket is the most sensitive indicator for impact angle and direction, and can show a "forbidden zone" on other terrestrial bodies.
The ejecta trajectories forming asymmetric or bilaterally symmetric ejecta blankets of oblique impacts may deviate from a radial orientation with respect to the final crater center and could probably be traced at the rim and overturned flap of simple craters, which represent the most proximal part of the ejecta. We therefore systematically analyzed strike and dip of strata in the crater rims of two young, simple impact craters, Wolfe Creek Crater and Meteor Crater.
Wolfe Creek Crater is located in Western Australia, was formed 300 ka ago and has an average diameter of 880 m. It was formed in sub-horizontal Devonian sandstones that are overlain by a layer of Miocene laterites. Meteor Crater in Arizona is 50 ka old and 1200 m in diameter. Pre-impact target rocks are sub-horizontal Permo-Triassic sandstones and limestones.
The strike data collected in both craters is translated from a geographic to an azimuthal referece scheme with the point of origin situated in the crater center. The strike of rock layers in the rim is examined for deviations from a hypothetical concentric orientation with regards to the crater center. The deviation can be expressed as an angular value for each measurement.
Results: When displayed in a polar plot, which gives a better sense of the spatial relationship, the values reveal a bilaterally symmetric orientation of the bedding and potential "forbidden zones". These preliminary results contradict earlier propositions for an impact vector in both Wolfe Creek Crater (Shoemaker et al., 2005) and Meteor Crater (Roddy & Shoemaker 1995). We intend to compare these results with other information, e.g. distribution of dip data, stereo plots and spatial relationships of bedding in three dimensions.
Acknowledgements: We would like to thank DFG for funding this project (KE 732-11/1).
(M. Poelchau, T Kenkmann and D. Kring, 2007)


(M come Meteorite - Matteo Chinellato)


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(Grieve R.A.F., Garvin J.B., Coderre J.M., Rupert J., 1989).

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(Shoemaker E.M., Shoemaker C.S., Nishiizumi K., Kohl C.P., Arnold J.R., Klein J., Fink D., Middleton R., Kubik P.W., Sharma P., 1990).

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(Blumberg D.G., McHone J.F., Kuzmin R., Greeley R., 1995).

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: Liverpool, Wolfe Creek, Boxhole, Veevers Dalgaranga. . ( ), .
(Shoemaker E.M., Macdonald F.A., Shoemaker C.S., 2005).




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