Figure 114

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 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
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