Show simple item record Wallis, D. Burchell, M. J. Cook, Anthony Solomon, C. J. McBride, N. 2008-12-09T15:01:42Z 2008-12-09T15:01:42Z 2005-05-21
dc.identifier.citation Wallis , D , Burchell , M J , Cook , A , Solomon , C J & McBride , N 2005 , ' Azimuthal Impact Directions from Oblique Impact Crater Morphology ' Monthly Notices of the Royal Astronomical Society , vol 359 , no. 3 , pp. 1137-1149 . DOI: 10.1111/j.1365-2966.2005.08978.x en
dc.identifier.issn 0035-8711
dc.identifier.other PURE: 89534
dc.identifier.other PURE UUID: cdbb77a2-a088-49ea-97e3-c96dc79f2ccc
dc.identifier.other dspace: 2160/1489
dc.identifier.other DSpace_20121128.csv: row: 1137
dc.identifier.other Scopus: 19844375495
dc.description Cook, Anthony; Wallis, D.; Burchell, M.J.; Solomon, C.J., (2005) 'Azimuthal Impact Directions from Oblique Impact Crater Morphology', Monthly Notices of the Royal Astronomical Society 359(3) pp.1137-1149 RAE2008 en
dc.description.abstract Planetary impact craters have a high degree of radial symmetry. This hampers efforts to identify the azimuthal impact direction for most craters – the radially symmetric component of an impact crater swamps any asymmetries that may be present. We demonstrate how the asymmetric component can be isolated and the direction of the asymmetries quantified using a two-dimensional eigenfunction expansion over a circular domain. The complex coefficients of expansion describe the magnitude and phase (angular alignment) of each term. From the analysis of hypervelocity impact craters formed in the laboratory, with impact angles ranging from 0° to 50° from the surface normal, we show that asymmetries which reveal the impact direction are still present at just 10° from the surface normal, and that the phase of one complex coefficient of expansion, c11, indicates the impact direction. Analysis of the lunar crater Hadley shows bilateral symmetry in the radially asymmetric component, which may be due to oblique impact. The 31-km lunar ray crater Kepler has morphological features that indicate the azimuthal impact direction. Coefficient c11 gives an azimuthal impact direction similar to that expected from the morphology, although post-impact gravitational collapse and slumping obscure the result to some degree. Ray craters may provide a means of testing the method for smaller 'simple' craters when data are available. en
dc.format.extent 13 en
dc.language.iso eng
dc.relation.ispartof Monthly Notices of the Royal Astronomical Society en
dc.rights en
dc.subject methods: laboratory en
dc.subject methods: numberical en
dc.subject comets: general en
dc.subject minor planets en
dc.subject asteroids en
dc.subject Moon en
dc.title Azimuthal Impact Directions from Oblique Impact Crater Morphology en
dc.type /dk/atira/pure/researchoutput/researchoutputtypes/contributiontojournal/article en
dc.contributor.institution Department of Physics en
dc.contributor.institution Mathematics and Physics en
dc.description.status Peer reviewed en

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