Publications

The lunar surface orientations of some of the Apollo 17 rock samples at the time of their collection (table 6-V) are shown in this appendix (figs. 6-65 to 6-87). These orientations were determined by correlating lunar photographs of samples before collection with shapes and shadow characteristics of the same samples in the LRL under oblique illumination with nearly collimated light. The...

Lunar slope-frequency distributions obtained by photogrammetric techniques are compared with results from the bistatic-radar investigations of the Apollo 14, 15, and 16 missions (refs. 33-16, 33-17, and 33-32) and of Explorer 35 (ref. 33-27). Algebraic standard deviations of slope-frequency distributions from photogrammetric data are equivalent to rms slopes of slope-frequency...

Apollo 17 metric photographs (fig. 29-26) provide the best available coverage for geologic interpretation of northern Mare Crisium and the northern Crisium basin. The area was covered previously by low-resolution telescopic and Lunar Orbiter IV photographs and by oblique, high-illumination, or low-resolution photographs from earlier Apollo missions. One region in particular, between...

A large quantity of data on backscattered polarized and depolarized radar echoes from the Moon has been collected from Earth at 3.8-cm wavelength (ref. 33-23). Depolarized echoes are particularly interesting because theory indicates that relatively strong depolarized echoes can be caused by the following factors.

No abstract available.

Small volcanic cones with summit craters or breached walls occur in several areas on the Moon. Most of these features have basal diameters of approximately 1 to 2 km and probably are not more than a few hundred meters in height. None have been so clearly photographed, however, as those shown in Apollo 17 metric and panoramic camera coverage of the southeastern margin of the Serenitatis...

A dark-colored surficial deposit covers lowlands and highlands along the southeastern margin of the Serenitatis basin. Sampling of this material was a major exploration objective of the Apollo 17 mission. Since completion of the mission, the dark mantle has been the subject of considerable controversy, inasmuch as no obvious stratified deposit was found in the landing area. Yet the...

The scientific objectives of the Apollo lunar sounder experiment (ALSE) are (1) mapping of subsurface electrical conductivity structure to infer geological structure, (2) surface profiling to determine lunar topographic variations, (3) surface imaging, and (4) measuring galactic electromagnetic radiation in the lunar environment. The ALSE was a three-frequency, wide-band, coherent radar...

Stereoscopic photographs taken by the metric and panoramic cameras can be used to obtain information on the roughness and slope-frequency distributions of lunar surfaces (see appendix to this part). Bistatic radar on board Apollo 14, 15, and 16 spacecraft may also be used to obtain information on lunar surface roughness at two wavelengths—13 cm (S-band) and 116 cm (VHF).

This catalog shows the locations from which samples were collected during the Apollo 17 mission and provides a descriptive geologic context for each sample. It is a working document principally of use to LSPET, LSAPT, and the lunar sample principal investigators. The information in this report is incomplete, but it is based on the best available data as of January 19, 1973. Sources of...

Orbital photographs taken at low-Sun illumination during both the Apollo 15 (ref. 30-14) and Apollo 17 missions have provided excellent data on the lava flows in the southwestern Mare Imbrium. These photographs have been used recently to present a detailed photogeologic evaluation of these flows and their role in mare volcanism of Eratosthenian age in the basin (ref. 30-15). Eruption of...

"Wrinkle ridges" in the Taurus-Littrow region along the eastern margin of the Mare Serenitatis appear very fresh and are probably among the youngest on the Moon. They include both mare ridges and similar-looking one-sided scarps. Evidence will be presented here to suggest that these ridges and scarps may be anticlines and thrust faults that resulted from sliding on a décollement surface