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.
Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
