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Morphology of martian rampart craters

Nature volume 272, pages 691694 (20 April 1978) | Download Citation

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Abstract

Preliminary results from a morphological analysis of the lobate flows around martian rampart craters are presented. The areal dispersal of these deposits displays a proportionally greater maximum range for the lobe as the size of the parent crater increases. It is proposed that lobe formation is not entirely associated with ballistic deposition of the crater's ejecta because the proximal ends of the lobes are found closer to the primary crater rim than to the region of secondary cratering associated with either lunar or mercurian craters. Lobe surface area is shown to be proportional to crater diameter and an estimate of 30–60 m is deduced for the lobe thickness for craters between 10 and 35 km diameter.

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Author notes

    • Peter J. Mouginis-Mark

    Present address: 26913 Cook Road, Olmsted Twp., Ohio 44138.

Affiliations

  1. Lunar and Planetary Unit, University of Lancaster, Lancaster, UK

    • Peter J. Mouginis-Mark

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DOI

https://doi.org/10.1038/272691a0

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