Abstract
A statistical model of cratered planetary surface has been developed in the case of i) primary impact events, ii) secondary-crater field. A test about the tendency to grouping of craters has been carried out in both cases by means of the method of the «strictly reflexive closeness» of the crater centres. The results obtained show the differences of behaviour, with respect to the grouping probability, between a population of fictitious primary craters and that including a secondary field. The method has been applied to actual planetary surfaces in order to check the influence of secondary events in crater statistics and to avoid it. Several crater surfaces on Mars and Mercury have been studied by this method allowing the identification of an upper limit for the value of the crater density (i.e. a lower limit for the crater diameter) useful to avoid the disturbance caused by the presence of secondary craters in a given area. This density (diameter) value obviously depends on the resolution of the available imagery.
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