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Chapter 2: Energy at the Lunar Surface - Lunar and Planetary Institute

Chapter 2: Energy at the Lunar Surface - Lunar and Planetary Institute

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Rock fragments more abundant<br />

West than typical mare<br />

- - East<br />

Outcrop.,.~p- ,<br />

Horizontal distance, m<br />

GRAVITATIONAL ENERGY<br />

Fig. 2.23. Diagram to illustr<strong>at</strong>e winnowing of lunar soil into a rille. Impacts on <strong>the</strong> rille rim eject<br />

m<strong>at</strong>erial in all directions but <strong>the</strong> rim receives ejecta from only one side. This results in a net movement<br />

of soil into <strong>the</strong> rille (after Swann et al., 1972).<br />

vicinity of <strong>the</strong> rim. In <strong>the</strong> narrow zone along <strong>the</strong> lip all cr<strong>at</strong>ers gre<strong>at</strong>er than<br />

0.5 m or so in diameter penetr<strong>at</strong>e <strong>the</strong> fine-grained m<strong>at</strong>erial, <strong>and</strong> <strong>the</strong>refore <strong>the</strong><br />

ejecta consist primarily of rock fragments. In <strong>the</strong> areas of normal soil<br />

thickness, only those cr<strong>at</strong>ers gre<strong>at</strong>er th<strong>at</strong> 20 to 25 m in diameter penetr<strong>at</strong>e<br />

<strong>the</strong> regolith, <strong>and</strong> even <strong>the</strong>n most of <strong>the</strong> ejecta are fine-grained m<strong>at</strong>erials from<br />

cr<strong>at</strong>ers approxim<strong>at</strong>ely 100 m in diameter. Therefore, <strong>the</strong> blocky n<strong>at</strong>ure of<br />

<strong>the</strong> 200 to 300 m zone along <strong>the</strong>'rille is due to <strong>the</strong> nearby source of rocks in<br />

<strong>the</strong> area of very thin soil along <strong>the</strong> rille rim.<br />

At <strong>the</strong> bottom of Hadley Rille, <strong>the</strong> fragment-size has a bimodal<br />

distribution (Fig. 2.24). Numerous large boulders have broken from <strong>the</strong><br />

outcrops <strong>at</strong> <strong>the</strong> rille rim <strong>and</strong> were large enough to roll over <strong>the</strong> fines to <strong>the</strong><br />

bottom. The rest of <strong>the</strong> m<strong>at</strong>erial is mainly fine grained <strong>and</strong> has probably<br />

been winnowed into <strong>the</strong> rille by cr<strong>at</strong>ering processes. Where <strong>the</strong> rille meets<br />

<strong>the</strong> pre-mare massif, <strong>the</strong> rille wall is made of fine-grained debris, <strong>and</strong> <strong>the</strong><br />

bottom of <strong>the</strong> rille is .shallower <strong>and</strong> fl<strong>at</strong>ter than elsewhere. This situ<strong>at</strong>ion<br />

indic<strong>at</strong>es a considerable fill of fine-grained debris derived from <strong>the</strong> massif.<br />

Mass movement is thus filling <strong>the</strong> rille <strong>and</strong> rounding <strong>the</strong> v-shape.<br />

Talus Slopes<br />

The Hadley Rille <strong>at</strong> <strong>the</strong> Apollo 15 l<strong>and</strong>ing site also offers <strong>the</strong> best<br />

inform<strong>at</strong>ion about talus slopes on <strong>the</strong> moon. The talus slopes th<strong>at</strong> form <strong>the</strong><br />

main walls of <strong>the</strong> rill& are blocky compared to most of <strong>the</strong> lunar surface (Fig.<br />

2.24). Loose debris is approxim<strong>at</strong>ely <strong>at</strong> <strong>the</strong> angle of repose. Boulder tracks<br />

visible on <strong>the</strong> slope of <strong>the</strong> rille wall indic<strong>at</strong>e recent instability of <strong>the</strong> blocks.

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