Preliminary geologic investigations of the Apollo 14 landing site

Revisiting the field geology of Taurus–Littrow

“…Down slope movement of continuously forming wall regolith would steadily expose additional large blocks along the rim crest and in the crater wall while blocks on the ejecta blanket were being ground into regolith. This is analogous to a similar process thought to be exposing fractured bedrock and boulders at the edge of Hadley Rille (Swann et al, 1972;Apollo Lunar Geological Investigation Team, 1972).…”

A volcanic origin for the outflow channels of Mars: Key evidence and major implications

“…(C) The head depression (arrow) of the 1200-kmlong Venusian outflow channel Kallistos Vallis; the channel continues southward from this depression, ultimately forming complex anastamosing reaches with widths of~30 km (Baker et al, 1992b) (e.g., Lingenfelter et al, 1968;Jones and Pickering, 2003;Waltham et al, 2008), volcanic interpretations are widely favored on the basis of the availability of relevant terrestrial analogs (e.g., Greeley, 1971aGreeley, ,b, 1977, the strong association of Venusian and lunar systems with volcanic landscapes (e.g., Wilhelms, 1987;Baker et al, 1992b), the anhydrous nature of associated geological materials (e.g., Goles et al, 1970;Keil et al, 1970;Swann et al, 1972;Papike et al, 1991;Nimmo and McKenzie, 1998), and the long-term instability of water at the surfaces of Venus and the Moon (Wilhelms, 1987;Papike et al, 1991). The properties of Rima Hadley, a lunar channel visited by astronauts during the Apollo 15 mission, are consistent with its development as a conduit for lavas of mafic composition (Greeley, 1971a;Howard et al, 1972;Swann et al, 1972;Carr, 1974). Eruption rates in excess of 1 × 10 4 to 1 × 10 6 m 3 /s are estimated to have been involved in the development of lunar channels and emplacement of mare flows (e.g., Schaber, 1973;Schaber et al, 1976), and corresponding eruption rates of up to~5 × 10 7 m 3 /s have been estimated for development of the largest Venusian channels .…”

Submillimeter-Scale Topography of the Lunar Regolith

“…The pictures were taken on and in the vicinity of "sloping rock," a gently sloping rocky surface that is seen in Apollo 14 Hassellblad picture AS14-68-9409 (Fig. 3) from a distance of about 15 m (Swann et al 1971).…”