Thickness determinations of the lunar surface layer from lunar impact craters

  • Quaide W
  • Oberbeck V
  • 28


    Mendeley users who have this article in their library.
  • N/A


    Citations of this article.


Small, fresh lunar craters with normal, central-mound, flat-bottomed, and concentric geometry are widespread on maria surfaces. The same types of craters have been produced in the laboratory by impacting projectiles against targets consisting of loose, granular, noncohesive materials overlying cohesive substrates. The mechanics of formation of each laboratory crater type is described, and evidence is offered that the corresponding types of lunar craters are of impact origin. Extensive studies of the effects of lunar impact variables on the conditions of formation of these crater types show that a previously described statistical method can be used to determine the thickness of the lunar surfaces layer within narrow limits. Two independent methods for determining the layer thickness at specific points are presented. Thickness estimates of the Surveyor 1 site obtained previously from study of medium-resolution Orbiter 1 photographs are re-evaluated by using subsequently obtained high-resolution photographs, and thickness determinations of two additional areas are presented. The different areas examined have different surface layer thickness. The fragments of the surface are certainly partly of impact origin, but volcanic contributions may also be present. The maria substrates are probably composed of volcanic flow rocks with interbeds of fragmental material.

Author-supplied keywords

  •, doi:10.

Get free article suggestions today

Mendeley saves you time finding and organizing research

Sign up here
Already have an account ?Sign in

Find this document


  • William L. Quaide

  • Verne R. Oberbeck

Cite this document

Choose a citation style from the tabs below

Save time finding and organizing research with Mendeley

Sign up for free