here for larger NASA image of Figure 91
Click here for larger NASA image of Figure 92
Click here for lunar chart showing location
The dark, rugged-surfaced complex of hills (V, at left) is enlarged many times in this stereogram. Without further detailed study, two explanations for its origin seem equally plausible. The complex may be a densely cratered block of terrae that was partly inundated by the lavas of Mare Cognitum and subsequently blanketed by dark volcanic ejecta. Within the darkened area, the concentration of fresh young craters is less than the surrounding mare surface, strongly suggesting that the dark blanketing was deposited appreciably later than the mare lavas.
Alternatively, the complex may be a pile of lava flows densely pockmarked
by volcanic craters, and, as in the first case, subsequently covered by
volcanic ejecta. The steplike, but discontinuous ledges along the east
side of the complex probably represent successive flows of viscous lava.
All the craters are shallow, probably because they have been filled by
their own ejecta or by that from nearby craters. Nevertheless, several
craters (see arrows) have steep raised rims, distinguishing them from impact
craters. The difference is clear at A where a volcanic crater (left) can
be readily compared to a normal impact crater (right). -G.W.C.
Report Source: NASA SP-362, Page 101, Figure 92
This web page was created by Francis Ridge
for The Lunascan Project
Section Directory 42