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Apollo 17 Mission (AS-5 12)
-- * Prelaunch Mission Operation Report No. M-933-72-17 28 November 1972 MEMORANDUM TO: A/Ad ministrator FROM: M/Apollo Program Director SUBJECT: Apollo 17 Mission (AS-5 12) . We plan to launch Apollo 17 from Pad A of Launch Complex 39 at the Kennedy Space Center no earlier than 6 December 1972. This will be the Apollo Program’s sixth and last manned lunar landing and the third consecutive mission to carry the Lunar Roving Vehicle for surface mobility, added Lunar Module consumables for a longer surface stay time, and the Scientific Instrument Module for extensive lunar orbital science investigations. Primary objectives of this mission are selenological inspection, survey, and sampling of materials and surface features in a preselected area of the Taurus-Littrow region of the moon; emplacement and activation of surface experiments; and the conduct of in-flight experiments and photographic tasks. In addition to the standard photographic documentation of operational and scientific activities, television coverage is planned for selected periods in the spacecraft and on the lunar surface. The lunar surface TV coverage will include remote controlled viewing of astronaut activities at each major science station on the three EVA traverses. The 12.7-day mission will be terminated with the Command Module landing in the mid-Pacific Ocean about 650 km (350 NM) southeast of Samoa Islands. ~P*h Rocco A. Petrone Manned Space Flight NOTICE: This document may be exempt from public disclosure under the Freedom of Information Act (5 U.S.C. 552). Requests for its release to persons outside the U.S. -
Subject Index
SUBJECT INDEX Accretion of the Moon Aphelion 34 (chemistry) 419 Apogee 57 Aeronautical Chart and Apollo 5, 8, 596–598, 602, 603, 605 Information Center Apollo 11 30, 609, 611–613 (ACIC) 60 geology 613 Age dating 134 landing site 611, 612 highland rocks 218, 219, 225, 228, 245, 250, Apollo 12 610, 614–616 253, 255, 256 geology 616 mare basalts 208, 209 landing site 614, 615 methods 134, 223 Apollo 14 31, 610, 617–619 Agglutinates 288, 296–299, 301, 339, 414 geology 619 and siderophile elements 414 landing site 617, 618 chemistry 299 Apollo 15 33, 36, 37, 337, 348, 620– description 296 622 F3 model 299 geology 622 genesis 298 heat flow 36, 37 mineralogy 297 landing site 620, 621 native Fe in 154 Apollo 16 32, 341, 351, 623–625, 631 petrography 298 geology 625 physical properties 296 landing site 623, 624 solar-wind elements in 301 Apollo 17 35, 37, 341, 348, 626–628, Akaganeite 150 631 Albedo 59, 558, 560, 561 geology 628 absorption coefficient 561 heat flow 37 Bond albedo 560 landing site 626, 627 geometrical albedo 560 Apollo command module normal albedo 560 experiments 596 scattering coefficient 561 Apollo Lunar Module (LM) 22, 476 single scattering albedo 560 Apollo Lunar Sample Return spherical albedo 560 Containers (ALSRC) 22 Albite 127, 363, 368 Apollo Lunar Sounder Aldrin, Edwin E., Jr. 27–30 Experiment (ALSE) 564 Alkali anorthosite 228, 381, 398, 399 Apollo Self-Recording high strontium, gallium Penetrometer (SRP) 508, 512, 591 content 399 Apollo Simple Penetrometer Alkali gabbro 370 (ASP) 506 Alkali gabbronorite 230, 368 Apollo -
3 2__ Cryptomarcdeposit
/,c, - c/C. ._; 3 2__ _d"/7--- Cryptomare Delineations using Craters as Probes to Lunar Stratigraphy: Use of Multispectral Clementine Data as a Tool; I. Antonenko, J. W. Head, C. M. Pieters. Dept. Geol., Brown Univ., Providence, RI 02912 USA, [email protected]. Hidden mare deposits, or cryptomare, present strong mafic component, and surprisingly, only a evidence of ancient mare volcanism [1], and thus merit portion of the wall of the large subdued crater appears furtherstudy. We have addressed issues of cryptomare to have a strong mafic component. identification [2], and presented techniques for Our analysis can be extended by considering 5- determining cryptomare geometry using dark halo channel spectra taken from key areas in the image. We impact craters (DHCs) which punch through overlying collectedaverage 3X3 pixel spectra for the locations ejecta to excavate underlying mare material [3]. These shown in Fig 1. Representative spectra of fresh techniques have been applied to a study area on the materials, gathered from the slopes of various small western limb of the Moon, using rectified Earth-based craters and in a traverse around the slopes of the large telescopic images and Zond data. The resolution and degraded crater, are shown in Fig 4: Craters whose coverage of these data sets, however, is fairly limiting. spectra exhibit a ferrous absorption feature near 1 gm Furthermore, visual identification of DHCs requires areinterlmm_astapping high-Ca pyroxene-rich that the soils developed on the crater ejecta be material indicating buried basalt (Fig 4A). Those that spectrally mature. The Clemenfine data set, with global exhibit a shorter wavelength absorption or a very weak coverage, improved resolution, and multiple channels, absorption are interpreted as tapping primarily highland presents a new opportunity to expand our studies, material (Fig 4B). -
The Geologic Investigation of the Taurus-Littrow Valley: Apollo 17 Landing Site
The Geologic Investigation of the Taurus-Littrow Valley: Apollo 17 Landing Site GEOLOGICAL SURVEY PROFESSIONAL PAPER 1080 THE GEOLOGIC INVESTIGATION OF THE TAURUS-LITTROW VALLEY: APOLLO 17 LANDING SITE By EDWARD W. WOLFE, NORMAN G. BAILEY, BAERBEL K. LUCCHITTA, WILLIAM R. MUEHLBERGER, DAVID H. SCOTT, ROBERT L. SUTTON, and HOWARD G. WILSHIRE ABSTRACT canic ash form an unconsolidated surficial deposit with an average thickness of about 14 m, sufficiently thick to permit abnormally rapid degradation of the smaller Astronauts Cernan and Schmitt, of Apollo 17, landed in the Taurus-Littrow valley craters, especially those less than 200 m in diameter, so as to create a surface that of the Moon on December 11,1972. Their major objectives were (1) to sample very appears less cratered than other mare surfaces. Admixed volcanic ash gives the ancient lunar material such as might be found in pre-Imbrian highlands as distant as surface a distinctive dark color, which, in combination with the less cratered possible from the Imbrium basin and (2) to sample pyroclastic materials that had appearance, led to its interpretation before the mission as a young dark mantling been interpreted as significantly younger than the mare basalts returned from unit. previous Apollo landing sites. The crew worked approximately 22 hours on the lunar The uppermost part of the regolith over much of the landing area is basalt-rich surface; they traversed about 30 km, collected nearly 120 kg of samples, took more ejects from the clustered craters of the valley floor. Most of the valley-floor craters than 2,200 photographs, and recorded many direct geologic observations.