here for larger NASA image
Click here for lunar chart showing location
This is an oblique view of another crater that probably was formed
by a meteoroid following a relatively low-angle trajectory. This crater,
4 km in diameter, is located in the highlands east of Mare Serenitatis.
Compared to the crater just described (see Figure
113 ), this one is less elliptical and its bilobate ray pattern
is much less pronounced. The differences may be attributed to a higher
trajectory angle of the impacting body that formed this crater as it struck
the surface. H. J. Moore (1976), in his study of craters formed by impacting
missiles at White Sands Missile Range, recognized a characteristic asymmetric
profile along the axis of trajectory for craters formed in this manner.
The wall beneath the missile trajectory is typically less steep than the
opposite or down-trajectory wall, and its rim crest is lower and more rounded.
These observations, when applied to the lunar crater in this photograph,
indicate that the impacting body was traveling toward the east when it
struck the Moon. -H.M.
Report Source: NASA SP-362, Page 120, Figure 114
This web page was created by Francis Ridge
for The Lunascan Project
Section Directory 25