Apollo 14: Preliminary Science ReportScientific and Technical Information Office, National Aeronautics and Space Administration, 1971 - Apollo Lunar Surface Experiments Package - 309 pages "Apollo 14, the third mission during which men have worked on the surface of the Moon, was highly successful. This mission to the Fra Mauro Formation provided geophysical data from a new set of instruments ... Because of improved equipment, such as the modularized equipment transporter, and because of the extended time spent on the lunar surface, a large quantity and variety of lunar samples were returned to Earth for detailed examination. New information concerning the mechanics of the lunar soil was also obtained during this mission. In addition, five lunar-orbital experiments were conducted during the Apollo 14 mission, needing no new equipment other than a camera. The experiments were executed by the command module pilot in the command and service module while the commander and the lunar module pilot were on the surface of the Moon. This report is preliminary in nature; however, it is meant to acquaint the reader with the actual conduct of the Apollo 14 scientific mission and to record the facts as they appear in the early stages of the scientific mission evaluation. As far as possible, data trends are reported, and preliminary results and conclusions are included."--Page xi. |
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12 sites abundant ALSEP amplitude analyzer angle Apollo 14 LM Apollo 14 mission Apollo 14 PSE appears approximately astronauts basaltic blocky boulders breccia camera CCGE clastic rock clasts Cone Crater core tube CPLEE crystalline dark deployed depth Descartes Crater detected detector diameter Earth ejecta blanket electrons energy fillet fine-grained flux foil Fra Mauro Formation fractures fragmental rocks frequency gegenschein geologic geophone grains Hasselblad indicate instrument King Crater layer LM ascent LM impact Lunar Orbiter lunar samples lunar soil lunar surface m/sec magnetic field magnetospheric mare material matrix Mauro Formation measured ment meteoroid module Moon moonquakes NASA observed particles percent photographs plagioclase range ratio recorded regolith retroreflector rock sample second EVA seismic signals seismometer shown in figure slope solar wind spacecraft station Theophilus Crater thermal thumper tion traverse trench values variations velocity waves zap pits
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Page 184 - N.; et al.: Trapped Solar Wind Noble Gases, Exposure Age and K/Ar Age in Apollo 11 Lunar Fine Material. Proceedings of the Apollo 11 Lunar Science Conference, Supp.
Page 220 - System noise temperature in this configuration is near 30° K when the antenna is aimed at the sky alone and 192° K when the Moon fills the beam of the antenna. The vhf receiving facility was the I50-ft parabolic antenna at the Stanford Center for Radar Astronomy.
Page 265 - Systems (SI) units used in this report and the numerical factors for converting from SI units to more familiar units. Names of International Units Used in This Report...
Page 220 - Center personnel, the receivers are tuned so that the direct signal will be centered in the passband at the time the CSM crosses the Earth-Moon line. The closed-loop receiver is initially tuned according to the operational-frequency predictions for the CSM. Once lock is achieved, the receiver automatically compensates for Doppler effects. Two magnetic-tape recorders are used simultaneously for data recording. Tapes are started at different times so that overlapping records (with no gaps for tape...
Page 217 - ... for a perfectly conducting sphere. The inferred reflectivity is then compared with the reflectivity of a dielectric surface under oblique geometry. The effective dielectric constant of the surface may be determined directly from the observation of the Brewster angle and indirectly by a quantitative comparison of the reflectivity values. The bandwidth of the echo depends directly on the surface slope. For the surface model considered previously, the bandwidth is given by...
Page 220 - NASA 36-bit time code and a synchronizing waveform, both of which are multiplexed onto the data tracks of the tape recorder. The two receiver channels, for right and left circular polarization, are sampled simultaneously so that the coherence between channels is preserved. Calibration signals are recorded, sampled, and processed in the same manner as the data. Weighted Fourier coefficients are computed using fast Fourier transform techniques.
Page 217 - ... first Fresnel zone, which is the specular point on the mean lunar surface. In ray-optics terminology, this is the point at which the angles of incidence and reflection are equal. If the Moon were a perfectly smooth sphere, all the echo would originate from a Fresnelzone-size spot surrounding this point. By roughening the surface through the introduction of large-scale (with respect to a wavelength) topographic undulations, this spot is caused to break up into a number of glints. The location...
Page 192 - One possibility is that the region was subjected to a uniform magnetic field but that various materials with differing coercivities were magnetized to different strengths. Another model might involve a slow variation in the direction of the ambient...
Page 260 - HOWARD, KA: Geologic Map of Part of the Apennine-Hadley Region of the Moon. Apollo 15 Premission Map. US Geol. Survey Map 1-723, 1971.
Page 265 - Area Volume Frequency Density Velocity Angular velocity Acceleration Angular acceleration Force Pressure Kinematic viscosity Dynamic viscosity Work, energy, quantity of heat Power Electric charge Voltage, potential difference, electromotive force Electric field strength Electric resistance Electric capacitance Magnetic flux Inductance Magnetic flux density Magnetic field strength Magnetomotive force Luminous...