apollo over the moon: a view from orbit (nasa sp-362)

Their cameras photographed almost the entire lunar surface (Kosofsky and El-Baz, 1970; NASA Langley Research Center, 1971). The coordinated operation of the three components of the mapping camera system is schematically illustrated in Figure 3. During normal photographic operations, the terrain camera automatically takes a series of photographs of the lunar surface.

Thus, the orientation of the latter (as well as the spacecraft) can be determined from the known position of the stars recorded by the star camera. The panoramic camera provided high-resolution stereoscopic coverage of large areas of the Moon's surface. The very dark objects at the bottom of the photo are large reels of film.

The final plans incorporated many of the recommendations made by the Apollo Orbital Science Photographic Team. Some of the experiments were conducted with the SIM bay pointed away from the Moon. The experiment thus provides a means to measure the small-scale "roughness" of the lunar surface.

One of the notable achievements of the Apollo program is the radiometric dating of returned samples, which shows that they are very old. Wilhelms graphically summarizes the order in which the major rock types of the lunar surface accumulated. The results of several Apollo experiments have confirmed their essential difference (Fig. 15).

TABLE 1.- Camera Systems Carried on Board the Command and Service Module (CSM) on Apollo Lunar Missions 8 Through 17

A true understanding of the evolution of the lunar crust may require years of additional study. The mechanics of impact crater formation has been intensively studied using Apollo data. Craters range in size from gigantic basins hundreds of kilometers in diameter (such as the Imbrium basin), to the smallest craters visible in orbital photographs (1 m in diameter), to microcraters on the surface of tiny glass beads contained in returned samples of lunar soil. were investigated.

Material from the eruption of craters has been studied and classified into two groups: ballistic ejecta, which is ejected to form linear or curved patterns of rays and clusters of secondary craters on the lunar surface, and fine-grained fluidized ejecta, which locally covers the lunar surface and forms patterned flows , extending down from the primary [27] impact crater. The continuous ejecta blanket is apparently deposited by the underlying shock flow on the surface surrounding the crater. A striking example of the surface patterns created by the ejecta flow and its interaction with the local topography is found near King Side Crater (Fig. 159).

Continued bombardment of the lunar surface by meteoroids and secondary impact material has formed a surface regolith composed of breccia fragments and unconsolidated fragmental debris. Dark halo craters have been extensively studied and are divided into two classes: round, smooth-sided craters with no visible blocks on the crater walls are believed to be volcanic, and dark halo material is thought to consist of very fine volcanic . extraction. Crater lines or chains are also classified into two groups: volcanic crater chains (Hyginus Rille and Davy crater chain) and secondary impact crater chains extending radially from large craters (such as Copernicus, Kepler and Aristarchus ) and formed by ballistic ejections from large craters.

Esenwein at NASA Headquarters provided much of the initial encouragement and support needed to begin this effort. Geological Survey and Farouk El-Baz of the Smithsonian Institution participated in the preliminary selection of the photos. Geological Survey compiled and edited the overlays according to the many preliminary versions of the book.

Goodrich and Mary Nelson Rakow of the Smithsonian Institution also assisted with many editorial tasks. We thank all the people associated with the Apollo missions; their hard work and technical expertise led to the acquisition of data that made this book possible.

APOLLO OVER THE MOON: A VIEW FROM ORBIT (NASA SP-362)

1st successful Ranger mission; impacted the Moon after taking 4,308 images of the lunar surface during its approach. 4 May 1967 Atlas-Agena D Photographed entire near side; after returning 326 images from orbit, collided with the Moon. A successful soft landing; 30,065 images and chemical and mechanical soil studies provided; made the first rocket launch to the moon.

The LM detached from the CM and piloted within 14.9 km of the Moon and returned to the CM; first color television from space (astronauts Stafford Young and Cernan). 1st manned lunar landing July 20, 1969 western Mare Tranquillitatus; 21.6 hours spent on the Moon; first samples of lunar rock returned to Earth (astronauts Armstrong Aldrin and Collins). Attempted manned landing mission aborted 56 hours after launch; returned after crossing the other side of the Moon (astronauts Lovell, Swigert and Liaise).

4th manned landing on 30 July 1971, Apennines-Hadley site in eastern Mare Imbrium; first manned lunar roving vehicle; SIM allowed a greater number of scientific experiments and more advanced photography to be conducted from orbit. 7, 1972 Saturn V program, Taurus-Littrow region; 79 hours on the lunar surface; 113 kg of rock samples returned to Earth (astronauts Cernan, Schmitt and Evans). Successful soft landing achieved in Le Monnier crater; automated roving vehicle Lunokhod 2 traveled 37 km and conducted many experiments over 5 Mondays.

Successful soft landing was achieved on Mare Crisium;. sampling is prevented from damaging the rock drill;. conducted limited research until November Achieved successful soft landing on Mare Crisium;. The full core sample from the 2m depth was returned to Earth in August. This project was led by the Advanced Research Projects Agency and started by the US lunar projects led by the National Aeronautics and Space Administration.

In the control solution performed by the Defense Mapping Agency Aerospace Center, each track pass was.