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  • LUNAR AND PLANETARY EXPLORATION  (726)
  • Fisheries
  • 2020-2024
  • 1975-1979  (726)
  • 1976  (726)
  • 1
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    Earth-based studies (1976)
    In:  Other Sources
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    Publication Date: 2019-08-28
    Description: Theoretical understanding of geologic processes of all planets and satellites is the ultimate goal of comparative geologic studies, simply because it is not possible to sample and study all bodies in the solar system in situ. Theories must make verifiable predictions, be able to test the aptness of terrestrial analogs, and ultimately should provide direction for future planetary research.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: A Geol. Basis for the Exploration of the Planets; p 85-106
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  • 2
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    The Venusian surface (1976)
    In:  Other Sources
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    Publication Date: 2019-08-28
    Description: Numerous questions generated by past Soviet and U.S. Venus missions regarding the climate and history of Venus have stimulated the initiation of a new U.S. program of Venus probes and orbiters. Among the issues that these missions are intended to resolve are the intensity of sunlight reaching the surface of the planet, the extent and composition of the cloud layer, and the mechanisms responsible for the extremely high surface temperatures measured by earlier probes. Also of interest are the reasons for the sharply differing terrains revealed by the Soviet probes Venera 9 and 10. Clarification of such questions may be expected to improve understanding of the origin of life on earth.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Natural History; 85; June-Jul
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  • 3
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    An inside look at NASA planetology (1976)
    In:  Other Sources
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    Publication Date: 2019-08-28
    Description: Staffing, financing and budget controls, and research grant allocations of NASA are reviewed with emphasis on NASA-supported research in planetary geological sciences: studies of the composition, structure, and history of solar system planets. Programs, techniques, and research grants for studies of Mars photographs acquired through Mariner 6-10 flights are discussed at length, and particularly the handling of computer-enhanced photographic data. Scheduled future NASA-sponsored planet exploration missions (to Mars, Jupiter, Saturn, Uranus) are mentioned.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Sky and Telescope; 51; Jan. 197
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  • 4
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    Viking Mars encounter (1976)
    In:  CASI
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    Publication Date: 2019-08-28
    Description: Various phases of planetary operations related to the Viking mission to Mars are described. Topics discussed include: approach phase, Mars orbit insertion, prelanding orbital activities, separation, descent and landing, surface operations, surface sampling and operations starting, orbiter science and radio science, Viking 2, Deep Space Network and data handling.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-76-116
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  • 5
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    Vikings converge on Mars (1976)
    In:  CASI
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    Publication Date: 2019-08-28
    Description: The scientific goals of the Viking mission are described. The science investigations to be carried out are explained and a timetable of planetary operations is outlined. Descriptions of the Viking orbiter and lander systems are presented including explanations of the Viking experimental instrument subsystems.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-76-103 , P76-10101
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  • 6
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    Reports of accomplishments of planetology programs, 1975 - 1976 (1976)
    In:  CASI
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    Publication Date: 2019-08-28
    Description: Abstracts of reports which summarize work conducted by Planetology Program Principal Investigators are presented. Full reports of selected abstracts were presented to the annual meeting of Planetology Program Principal Investigators at the Center for Astrogeology, U.S. Geological Survey, Flagstaff, Arizona, March 8, 9, 19, 1976.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-X-3364
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  • 7
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    Hydrogen resources for the moon (1976)
    In:  CASI
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    Publication Date: 2019-08-28
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Inst., Abstracts of Papers Presented at a Special Session of the Seventh Annual Lunar Science Conference on Utilization of Lunar Materials and Expertise for Large Scale Operations in Space; p 55-60
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  • 8
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    What's new on the moon? (1976)
    In:  CASI
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    Publication Date: 2019-08-28
    Description: As a result of the Apollo program and other lunar probes, questions that remained unsolved during centuries of speculation and scientific study can now be answered concerning the composition, core, surface, age, and history of the moon. Data obtained from lunar samples and instruments on the lunar surface are being used to gain insight into the history of the earth and the other planets, planetary evolution, the development of planetary magnetic fields, the nature of the solar wind, and how the Sun operates. Projects suggested for using the moon to increase understanding of geophysics are described.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-EP-131
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  • 9
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    Viking on Mars - A preliminary survey (1976)
    In:  Other Sources
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    Publication Date: 2019-08-27
    Description: Selection of landing site, observations of Martian topography from orbit, a log of entry into the Martian atmosphere and landing operations, and soil experiments executed at the landing site are recounted. Several photographs overviewing Martian terrain from orbit (1600 to 1900 km up) are shown. Soil sampling and analysis experiments and experiments designed to detect biotic activity (pyrolysis, labeled release of 14-carbon-tagged CO2, gas exchange and vapor chromatography, pyrolytic release) are described and some preliminary results reported. Results on surface geology and chemical composition of the Martian atmosphere are cited.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: American Scientist; 64; Nov
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  • 10
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    Discoveries about Jupiter. Results for Pioneers 10 and 11 combined with earth-based findings (1976)
    In:  CASI
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    Publication Date: 2019-08-27
    Description: Included in this discussion of findings regarding the planet Jupiter are atmospheric characteristics, weather, the magnetosphere, radiation belts, radio emission, natural satellites, possible origins, the Great Red Spot, the interior and the possibility of life.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-76-91
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  • 11
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    The Surface Chemical Composition of Lunar Samples and Its Significance for Optical Properties (1976)
    In:  CASI
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    Publication Date: 2019-08-14
    Description: The surface iron, titanium, calcium, and silicon concentration in numerous lunar soil and rock samples was determined by Auger electron spectroscopy. All soil samples show a large increase in the iron to oxygen ratio compared with samples of pulverized rock or with results of the bulk chemical analysis. A solar wind simulation experiment using 2 keV energy alpha -particles showed that an ion dose corresponding to approximately 30,000 years of solar wind increased the iron concentration on the surface of the pulverized Apollo 14 rock sample 14310 to the concentration measured in the Apollo 14 soil sample 14163, and the albedo of the pulverized rock decreased from 0.36 to 0.07. The low albedo of the lunar soil is related to the iron + titanium concentration on its surface. A solar wind sputter reduction mechanism is discussed as a possible cause for both the surface chemical and optical properties of the soil.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-148169 , CRSR-634 , Lunar Sci. Conf.
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  • 12
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    The densities and bulk compositions of Ceres and Vesta (1976)
    In:  Other Sources
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    Publication Date: 2019-08-13
    Description: Present radiometric and polarimetric measurements of the sizes and albedos of asteroids 1 Ceres and 4 Vesta, although uncertain in absolute calibration, determine the ratio of diameters with sufficient precision (Ceres/Vesta = 1.87 plus or minus 0.03) to permit meaningful discussion of their relative densities. These measurements combined with the known masses yield a ratio of densities Vesta/Ceres = 1.33 plus or minus 0.17, thus demonstrating that: (1) the bulk compositions are likely different, and (2) the difference is consistent with indications from remotely-determined surface composition that Vesta is differentiated while Ceres may be of undifferentiated carbonaceous chondritic composition.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geophysical Research Letters; 3; Dec. 197
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  • 13
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    Micrometeorite penetration effects in gold foil (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Penetration structures revealed by a Skylab experiment dealing with exposure of single and double layers of 500-800 A thick gold foil to micrometeorites are examined. Examination of all double-layered gold foils revealed that particles producing holes of any type greater than 5 microns in diameter in the first foil break up into many fragments which in turn produce many more holes in the second foil. Evidence of an original particle is not found on any stainless steel plate below the foils, except in one instance. A precise relationship between the size of the event and the mass of the particle producing it could not be determined due to the extreme morphological variety in penetration effects. Fluxes from gold foil and crater experiments are briefly discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Symposium and Workshop on Results from Coordinated Upper Atmosphere Measurement Programs; May 29, 1975 - May 31, 1975|Open Meetings of Working Groups on Physical Sciences; May 29, 1975 - Jun 07, 1975; Varna; Bulgaria
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  • 14
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    Colloquium on Water in Planetary Regoliths, Hanover, N.H., October 5-7, 1976, Proceedings (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The papers abstracted in this volume deal with the occurrence, detection, and measurement of water on planetary bodies in the solar system; relevant aspects of the terrestrial water balance; the most probable status of water on other planetary bodies; and the methods of water detection and measurement available for consideration in designing planetary exploration missions. Topics include the water inventory for earth, high-energy protons as an early source of regolith water, the evolution of water on Mars, the chemical evolution of the Martian atmosphere by surface weathering, some geochemical aspects of excess volatiles on Mars, fluvial erosion on Mars, water in the outer solar system, and the stability of water on the Galilean satellites. Other papers discuss gamma-ray attenuation methods for determining the water content of soil, Viking biology-experiment results relevant to water on Mars, IR detection of water ice on satellite surfaces during the Mariner Jupiter/Saturn mission, electrical sounding of the lunar regolith, the detection of water on the moon and Mars by orbital gamma-ray spectroscopy, and the Viking Martian soil-water analyzer.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Water in Planetary Regoliths; Oct 05, 1976 - Oct 07, 1976; Hanover, NH; US
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  • 15
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    Absorption of radiation belt particles by the inner satellites of Jupiter (1976)
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    Publication Date: 2019-07-13
    Description: The study of trapped particle absorption by the inner Jovian satellites is reviewed from the viewpoint of radiation belt physics. Both pre- and post-Pioneer work is discussed but the emphasis is on methods used to deduce radial diffusion coefficients of particle transport from particle data. The phenomenon of particle absorption as observed by experiments on Pioneers 10 and 11 is considered; absorption effects are found to depend on the satellite, and on particle energy and species. Approximate diffusion coefficients derived from the data are found to follow a steeper spatial dependence than previously expected. The assumptions and limitations of absorption analysis and diffusion coefficient estimation are pointed out.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 16
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    Interior structure of Jupiter - Theory of gravity sounding (1976)
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    Publication Date: 2019-07-13
    Description: Using relatively simple interior models and a fourth-order theory of figures, it is found that there are basically two extremes of interior structure which agree with current gravity data. One extreme is a 'solar'-composition envelope with 10 to 15 earth masses of heavy material in a core; the other extreme has nearly uniform 'solar' composition but with approximately an additional 30 earth masses of heavy material distributed essentially uniformly. Thus, Jupiter is not of 'solar' composition. It is shown how additional gravity data and improvement in knowledge of the molecular hydrogen equation of state will permit a significant reduction in the number of possible models.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 17
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    Interior models of Jupiter (1976)
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    Publication Date: 2019-07-13
    Description: Understanding the interior of Jupiter depends upon our knowledge of the thermodynamics and transport properties of hydrogen-helium mixtures at high pressures and temperatures. The current status of this knowledge is reviewed, and attention is given to the metallic-molecular hydrogen transition and the limited solubility of helium in hydrogen. Models of Jupiter are constructed which are consistent with all the observations to date, but which make various assumptions about the thermodynamics and composition of the interior. These models typically consist of a rocky core surrounded by a nearly-solar fluid mixture. In contrast to the models of Podolak and Cameron, a large enhancement of water or helium is not found to be essential. It is concluded that further progress in constructing interior models requires a better understanding of the thermodynamics of dense molecular hydrogen.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 18
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    On the origin of the solar system and of Jupiter and its satellites (1976)
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    Publication Date: 2019-07-13
    Description: The evolution of the middle part of the primitive solar nebula is traced through seven stages: (1) a gravitational instability which clumps condensed material into bodies of appreciable size; (2) the formation of a larger body as a result of mutual collisions; (3) gravitational condensation of the gas in the nebula; (4) subsequent hydrodynamic collapse of the gas onto a heavy-element planetary core; (5) the attainment of a highly distended hydrostatic configuration and its subsequent slow gravitational contraction; (6) the formation of a gaseous disk around proto-Jupiter; and (7) the formation of the Galilean satellites (and Amalthea) within this disk. Different theories on the origin of the primitive solar nebula are reviewed, models of Jupiter are evaluated, and the origin and evolution of the planet are traced through the indicated stages. It is proposed that Jupiter's current excess luminosity is due mostly to a loss of internal energy generated during the initially more rapid contraction period and, to a lesser degree, to the planet's current release of gravitational energy. The question of when the icy constituent was added to the outer two Galilean satellites is considered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 19
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    The trapped radiation belts of Jupiter (1976)
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    Publication Date: 2019-07-13
    Description: The preliminary results from the Trapped Radiation Detector instruments of the University of California at San Diego aboard Pioneers 10 and 11 for making measurements in the Jupiter magnetosphere are reviewed. Attention is given to the instrument and the flyby trajectories and results of the following investigations are presented: interplanetary electrons of Jovian origin, the configuration of the magnetosphere, interactions between the trapped radiation belts and Jupiter's satellites, (absorption of trapped radiation, the effect of angular dimensions, and the injection of energetic radiation), the behavior of electrons in the inner Jupiter magnetosphere, and multiple peaks near Pioneer 11 periapsis.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 20
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    Dynamics of the Jovian magnetosphere and energetic particle radiation (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Inferences are drawn from Jovian magnetosphere data acquired in the flybys of Pioneer 10 and Pioneer 11. Data on the outer magnetosphere and the inner core, and on observed 10-hr variations in particle intensity, are summarized, with attention given to the immense size and complexity of the magnetosphere and the behavior of trapped charged particles. The data support the maintenance and acceleration of charged particles trapped in Jupiter's magnetic field by inward diffusion in violation of the third adiabatic invariant. Prodigious quantities of high-energy particles are found to escape from Jupiter into interplanetary space, and MHD waves in the circumjovian plasma are considered. Whether the 10-hr variations are spatial or temporal in origin is weighed in favor of the latter. Production and loss mechanisms for the particles, and the nature of the Jovian magnetosphere itself, are noted among questions remaining obscure.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 21
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    Earth-based radio observations of Jupiter - Millimeter to meter wavelengths (1976)
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    Publication Date: 2019-07-13
    Description: The historical development of the study of Jupiter radio emission is considered and a description of the observational data is presented, taking into account the spectrum of the continuous microwave radiation, the polarization of the microwave radiation, the brightness distribution, the rotation-related variability, variations related to the zenocentric declination of the earth, and other time variations. The separation of radio emission into thermal and nonthermal components is discussed and interpretations of the two components are provided. A comparison of earth-based radio measurements with Pioneer 10 and 11 data is conducted and the future of earth-based radio observations is evaluated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 22
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    Pioneer 10 ultraviolet photometer observations of Jupiter - The helium to hydrogen ratio (1976)
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    Publication Date: 2019-07-13
    Description: Pioneer 10 UV photometric observations of solar He I 584-A emissions diffusely reflected from the atmosphere of Jupiter are discussed which establish the expected presence of He in the planet. The intensity and profile of the solar He line are remeasured and found to be more intense than originally supposed, implying a lower value for the diffuse 584-A reflectivity of Jupiter and less He than previously estimated. Other measurements of the solar He line are reviewed, resonance scattering by He is analyzed, and radiative-transfer calculations for Jovian model atmospheres are improved by including the anisotropic phase function for helium resonance scattering. The assumption of coherent scattering in the formation of the Jovian airglow line is shown to be an accurate approximation, and present estimates of the atmospheric temperature and eddy diffusion coefficient are examined. An atmospheric He/H abundance ratio greater than zero but less than approximately 28% is determined by assuming an isothermal atmosphere with a temperature of 150 K and the range of eddy-diffusion values given by Pioneer 10 Ly-alpha observations. The effect of higher temperatures on the He/H abundance is briefly evaluated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 23
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    Chemistry and spectroscopy of the Jovian atmosphere (1976)
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    Publication Date: 2019-07-13
    Description: A comprehensive review is given of the chemistry and spectroscopic studies of the Jovian atmosphere. Thermochemical equilibrium models for determining atmospheric composition are considered along with possible disequilibrating processes, and studies of the photochemistry of H2, CH4, NH3, H2S, and PH3 using the modeling methods are summarized. It is shown that photodissociation and advection are the major disequilibrating processes in Jupiter's atmosphere, that lightning and charged-particle bombardment are relatively minor factors in the planet's bulk chemistry, and that the existence of living organisms on the planet is highly improbable. Spectroscopic investigations of Jupiter are discussed, emphasizing recent observations of absorption bands due to CH4, NH3, H2, He, and D. Spectroscopic abundance determinations are examined for H2, HD, CH4, CH3D, NH3, C2H6, C2H2, and PH3. Upper limits are given for the abundances of several unobserved gases in the visible atmosphere, including H2S, HCl, SiH4, benzene, purines, pyrimidines, and their derivatives.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 24
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    Structure of the atmosphere of Jupiter from Pioneer 10 and 11 radio occultation measurements (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: A technique for incorporating effects of the oblateness of Jupiter's atmosphere into the data analysis procedure for radio-occultation measurements is described which makes use of a spherical harmonic representation of the gravity field to compute the shape of the planet. With this technique, the center of refraction is located by the radius of curvature and the normal direction at the closest approach point of the ray. The present technique, a subsequent approximation involving the use of a constant center of refraction, and the Abel integral transform inversion method for spherical planets are applied to Pioneer 10 and 11 data. All the intermediate results obtained show a temperature inversion between 10 and 100 mb, with temperatures from 130 to 170 K at 10 mb and from 80 to 120 K at 100 mb. Comparison of the radio-occultation profiles with radiative-convective equilibrium models and the temperature profile based on Pioneer 10 IR radiometer data indicates good agreement between the models and the occultation results.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 25
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    The Pioneer 11 radio occultation measurements of the Jovian ionosphere (1976)
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    Publication Date: 2019-07-13
    Description: Radio occultation data obtained with the Pioneer 11 spacecraft are utilized to study Jupiter's ionosphere. The ingress measurements, which were conducted by using a stable earth-based frequency reference for the tracking link, yielded ionospheric data near the morning terminator at about 79 deg south latitude. Data were also taken during egress on the evening side near 20 deg north latitude. The latter measurements were conducted in the one-way mode; i.e., an on-board crystal oscillator was employed as a frequency reference for the downlink (spacecraft-to-earth) signal. These data confirm previous results obtained with Pioneer 10 and show that Jupiter has a multilayered ionosphere extending over an altitude range of more than 3000 km. The topside scale height near 79 deg south latitude was 540 + or - 60 km. Assuming a topside electron, H(+) distribution controlled by diffusion yields a plasma temperature of 850 + or - 100 K in this region. The radio data indicate that the upper atmosphere is either warmer or more dissociated into atomic hydrogen than previously anticipated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 26
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    The motions of satellites and asteroids - Natural probes of Jovian gravity (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Before the recent Pioneer probes, our knowledge of Jupiter's gravitational field was obtained from the motions of satellites and asteroids. The study of orbital perturbations of asteroids near the 2:1 commensurability yielded a value of the mass of the Jupiter system at least as precise as that obtained by the artificial probes. Precession of the inner satellites' orbits placed constraints on the harmonic coefficients J2 and J4. A correction to the satellite determination of J4 lowers its mean value closer to the Pioneer result. The orbital grouping among the outer satellites and the resonance among the Galilean satellites are described in detail, but the origins of these phenomena are not understood. However, recent research suggests that the explanation will be intimately associated with models of the origin and evolution of the planet itself.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 27
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    The Jovian meteoroid environment (1976)
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    Publication Date: 2019-07-13
    Description: Meteoroid fluxes in interplanetary space at 5 AU and near Jupiter have been measured with the penetration detectors on Pioneer 10 and Pioneer 11. The data suggest that the size distribution of meteoroids at 5 AU is the same as that at 1 AU. Furthermore, the high flux observed near Jupiter appears due to meteoroids in orbit about the sun being gravitationally focused toward the planet. There is no indication of a large population of particles in orbit around Jupiter. Calculations show that the mass influx of meteoroids on Jupiter is 170 times that on the earth, but this does not have a significant effect on the energy balance of Jupiter. The high speed with which meteoroids enter the Jovian atmosphere causes them to be brighter than those on earth so that the number of visible meteors is 5800 times the number in the earth's atmosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 28
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    Results of the plasma analyzer experiment on Pioneers 10 and 11 (1976)
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    Publication Date: 2019-07-13
    Description: The plasma-analyzer experiments on Pioneers 10 and 11 have determined that the characteristics of the solar-wind interaction with the Jovian magnetosphere are basically similar to those observed for the solar-wind interaction of earth and differ mainly in terms of the scale size of the interaction. The Jovian magnetosheath flow field and the calculated normals to the Jovian magnetosphere indicate that the Jovian magnetosphere is extremely thick and blunt in shape. The size of the Jovian magnetosphere in the sunward (dayside) direction can change by as much as a factor of two in response to relatively minor changes in solar-wind dynamic pressure. The outer dayside Jovian magnetosphere is inflated with a high-beta thermal plasma.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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    Results from the GSFC fluxgate magnetometer on Pioneer 11 (1976)
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    Publication Date: 2019-07-13
    Description: A high-field triaxial fluxgate magnetometer was mounted on Pioneer 11 to measure the main magnetic field of Jupiter. It is found that this planetary magnetic field is more complex than that indicated by the results of the Pioneer 10 vector helium magnetometer. At distances less than 3 Jupiter radii, the magnetic field is observed to increase more rapidly than an inverse-cubed distance law associated with any simple dipole model. Contributions from higher-order multipoles are significant, with the quadrupole and octupole being 24 and 21 percent of the dipole moment, respectively. Implications of the results for the study of trapped particles, planetary radio emission, and planetary interiors are discussed. Major conclusions are that the deviation of the main planetary magnetic field from a simple dipole leads to distortion of the L shells of the charged particles and to warping of the magnetic equator. Enhanced absorption effects associated with Amalthea and Io are predicted.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Colloquium on Jupiter: Studies of the interior, atmosphere, magnetosphere and satellites; May 19, 1975 - May 21, 1975; Tucson, AZ
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  • 30
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    Surface chemistry of selected lunar regions (1976)
    In:  CASI
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    Publication Date: 2019-07-13
    Description: A completely new analysis has been carried out on the data from the Apollo 15 and 16 gamma ray spectrometer experiments. The components of the continuum background have been estimated. The elements Th, K, Fe and Mg give useful results; results for Ti are significant only for a few high Ti regions. Errors are given, and the results are checked by other methods. Concentrations are reported for about sixty lunar regions; the ground track has been subdivided in various ways. The borders of the maria seem well-defined chemically, while the distribution of KREEP is broad. This wide distribution requires emplacement of KREEP before the era of mare formation. Its high concentration in western mare soils seems to require major vertical mixing.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-X-74611 , LA-UR-76-972 , CONF-760323-4 , Lunar Sci. Conf. on Util. of Lunar Mater. and Expertise for Large Scale Operations in Space; Mar 15, 1976 - Mar 19, 1976; Houston, TX; United States
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    Study of the ablative effects on tektites (1976)
    In:  CASI
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    Publication Date: 2019-07-13
    Description: Equations are presented which provide approximate parameters describing surface heating and tektite deceleration during atmosphere passage. Numerical estimates of these parameters using typical initial and ambient conditions support the conclusion that the commonly assumed trajectories would not have produced some of the observed surface markings. It is suggested that tektites did not enter the atmosphere singly but rather in a swarm dense enough to afford wake shielding according to a shock envelope model which is proposed. A further aerodynamic mechanism is described which is compatible with hemispherical pits occurring on tektite surfaces.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-152423 , AVSD-0104-76-CR
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  • 32
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    An investigation of the effects of mass loss, shape change and real gas aerodynamics on a Jovian atmospheric reconstruction experiment (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: A survey of the effects of mass loss, shape change and real-gas aerodynamics on a Jovian atmospheric reconstruction experiment is carried out. Techniques used to reconstruct atmospheric profiles from entry probe measurements are discussed and some of the parameters which affect their accuracy are identified. Trajectory analyses and real-gas, radiatively-coupled flow field analyses (which include the effects of mass loss and shape change) are carried out for several candidate probe configurations. From these analyses, uncertainties in the atmospheric reconstruction procedure are estimated. Finally, the prospects for reducing these uncertainties by optimizing probe configuration and by instrumentation of the probe heat shield to measure actual shape change are considered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: IAF PAPER 76-073 , International Astronautical Congress; Oct 10, 1976 - Oct 16, 1976; Anaheim, CA
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  • 33
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    Results of the asteroid-meteoroid particle experiment on Pioneer 11 (1976)
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    Publication Date: 2019-07-13
    Description: The Asteroid-Meteoroid Detector, an electro-optical instrument that detects and measures particles in space by sensing the sunlight reflected from them, is part of the payload of both the Pioneer 10 and 11 spacecraft. The Pioneer 11 instrument is essentially identical to that on Pioneer 10, with some minor modifications. Reduction of the Pioneer 11 data was complicated by the failure of one of the four sensor channels at about 1.1 AU from the sun. Detailed analysis yielded 51 events between 1.0 and 3.5 AU, which were used to determine the particle concentration distribution in that region of space. Weighted curve-fitting of the results shows agreement with the concentrations derived from Pioneer 10 to within about a factor of two. As with the Pioneer 10 results, the exponent of the size dependency varies from about -1.7 for 100-micron radius particles to about -3.2 for 10-cm bodies. The instrument, its operation, and the method of data analysis are reviewed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: COSPAR, Plenary Meeting; Jun 08, 1976 - Jun 19, 1976; Philadelphia, PA
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  • 34
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    Electrostatic disruption of lunar dust particles (1976)
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    Publication Date: 2019-07-13
    Description: The possibility that dust particles might explode catastrophically on the lunar surface due to electrostatic charging is examined. For the dark side along the terminator zone, dust balls and compact stony particles of micron and submicron sizes will be blown up if their surface potential is as low as a kilovolt negative. This mechanism does not operate on the sunlit side because the surface potential is only 3.5-20 volts positive.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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  • 35
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    Lunar soil movement registered by the Apollo 17 cosmic dust experiment (1976)
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    Publication Date: 2019-07-13
    Description: The paper describes the Lunar Ejecta and Meteorites (LEAM) experiment of the Apollo 17 flight mission, placed in the Taurus-Littrow area of the moon. The objective of the experiment was to measure impact parameters of cosmic dust on the lunar surface. Preliminary data analysis led to the recognition that the bulk of events recorded by the LEAM experiment are not signatures of hypervelocity cosmic dust particles as expected, but are induced signatures of electrostatically charged and transported lunar fines.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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  • 36
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    The size frequency distribution and rate of production of microcraters (1976)
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    Publication Date: 2019-07-13
    Description: The paper contends that lunar crater size distributions vary to a degree that cannot be explained by variations in lunar surface orientation of the crater detectors or changes in micrometeoroid flux. In an attempt to investigate this size frequency distribution, a flux of micrometeoroid particles producing 0.1 micron diameter craters of approximately 300/sq cm/steradian/yr was obtained. No anisotropy was observed in the 0.1 micron flux between the ecliptic plane and the normal in the direction of lunar north.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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  • 37
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    Dust in the outer solar system - Review of early results from Pioneers 10 and 11 (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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  • 38
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    Lunar microcraters and interplanetary dust fluxes (1976)
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    Publication Date: 2019-07-13
    Description: Conflicting depth/diameter ratios reported for lunar microcrater pits, microcrater pit morphology and size distribution, the composition and structure of pit glasses, and various alternative 'clocks' for estimating exposure time of microcrater pits are examined. Surface exposure time 'clocks' discussed include: galactic cosmic ray tracks, cosmogenic nuclides (involving changes in host rock isotopic composition induced by nuclear reactions), tracks produced in lunar top surfaces by nuclei accelerated during solar flares, and solar wind sputtering. 'Calibration' of the disparate types of surface exposure time 'clocks' with one another is discussed. The sensitive relationship between determinations of meteoroid flux and surface exposure time is examined.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Interplanetary dust and zodiacal light; Jun 10, 1975 - Jun 13, 1975; Heidelberg
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  • 39
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    Spherical harmonic representation of the gravity field of Mars using a short-arc technique (1976)
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    Publication Date: 2019-07-13
    Description: Planetary gravity fields are primarily determined from Doppler tracking of orbiting spacecraft which are typically in high eccentricity orbits. Thus, the non-central gravitational components perturb the orbit primarily in the vicinity of periapsis. To find a computationally efficient technique and to reduce the influence of unmodeled forces on the spacecraft, an analysis has been performed of the effectiveness of processing only data in the vicinity of periapsis using multiple short arcs. Mariner 9 data are processed for the study, using 1, 2, 3 and 4 hour arcs and estimating gravity fields from 4th through 7th degree. The resulting gravity fields are inter-compared and also compared with previously published results.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: AIAA PAPER 76-823 , Astrodynamics Conference; Aug 18, 1976 - Aug 20, 1976; San Diego, CA
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  • 40
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    Lunar radargrammetry with ALSE-VHF imagery (1976)
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    Publication Date: 2019-07-13
    Description: Results are presented for a controlled experiment with a pair of overlapping lunar ALSE-VHF images produced in two consecutive revolutions of the Apollo command module around the moon. A theoretical treatment is presented of the mathematical tools for ALSE radargrammetry. Evaluation of radargrammetric mapping with single strips and a radar stereo model led to preliminary results in a test area around Mons Maraldi. Accuracy achieved with single radar images was about plus or minus 250 m along track and plus or minus 500 m across track. Stereoradargrammetry was used to generate a contour plot of Mons Maraldi and to evaluate the overall height accuracy obtainable from ALSE radar. About plus or minus 120 m of accuracy is obtained if the stereo model is corrected using a few control points. This makes ALSE stereo radar heights competitive with or even superior to vidicon data obtained for planetary exploration. The present basic limitation to radargrammetric accuracy from ALSE-VHF images is the identifiability of surface features.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Fall Convention; Oct 26, 1975 - Oct 31, 1975; Phoenix, AZ
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  • 41
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    Applied photo interpretation for airbrush cartography (1976)
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    Publication Date: 2019-07-13
    Description: Lunar and planetary exploration has required the development of new techniques of cartographic portrayal. Conventional photo-interpretive methods employing size, shape, shadow, tone, pattern, and texture are applied to computer-processed satellite television images. Comparative judgements are affected by illumination, resolution, variations in surface coloration, and transmission or processing artifacts. The portrayal of tonal densities in a relief illustration is performed using a unique airbrush technique derived from hill-shading of contour maps. The control of tone and line quality is essential because the mid-gray to dark tone densities must be finalized prior to the addition of highlights to the drawing. This is done with an electric eraser until the drawing is completed. The drawing density is controlled with a reflectance-reading densitometer to meet certain density guidelines. The versatility of planetary photo-interpretive methods for airbrushed map portrayals is demonstrated by the application of these techniques to the synthesis of nonrelief data.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Fall Convention; Oct 26, 1975 - Oct 31, 1975; Phoenix, AZ
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  • 42
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    Physical properties of asteroids from UBV photometry (1976)
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    Publication Date: 2019-07-13
    Description: A program of asteroid photoelectric photometry is discussed which is designed primarily to obtain UBV magnitudes and colors of most asteroids reaching magnitude 13.3 or brighter at opposition and of asteroids reaching magnitude 14.3 or brighter at perihelic opposition. A two-color plot is presented for asteroids whose compositional classes have been determined by radiometry, spectrophotometry, and polarimetry. A clear separation by color is observed for S and C objects; M and E objects are shown to be colorimetrically similar to C objects. Another two-color plot for about 200 asteroids reveals a continuum between the C and M, E domains and a possible continuum between the C and S domains. A plot of the frequency distribution of asteroid semimajor axes indicates that C objects predominate in the outer part of the asteroid belt while S objects are more numerous in the inner part. Statistics of asteroid phase angles and light-curve amplitudes are examined. It is suggested that the phase coefficient of an asteroid is inversely proportional to its geometric albedo and that S objects may be less spherical than C objects.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Annual Meeting; Mar 30, 1976 - Apr 03, 1976; Austin, TX
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  • 43
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    Far infrared spectral observations of Venus, Mars and Jupiter (1976)
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    Publication Date: 2019-07-13
    Description: Far-IR spectra of Venus, Mars and Jupiter between 46 and 115 microns have been obtained at a resolving power of about 10, observing from the NASA Lear Jet at an altitude of 13.7 km. The results are calibrated with lunar observations and show Mars and Venus to have relatively constant brightness temperatures over this wavelength region, with Venus appearing somewhat warmer at longer wavelengths. The brightness temperature of Jupiter decreases slightly toward longer wavelengths.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: COSPAR, Plenary Meeting; Jun 08, 1976 - Jun 19, 1976; Philadelphia, PA
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  • 44
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    The magnetosphere of Mercury (1976)
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    Publication Date: 2019-07-13
    Description: Data on Mercury's magnetosphere and on the plasma, planetomagnetic, and energetic particle environment of the planet obtained in three encounters (Mariner 10 flybys) are compared, and tasks for future research are outlined. The Mercury bow shock and magnetopause are much closer to the planet than the earth counterparts are to the earth. The magnetotail with embedded plasma sheet-field reversal region, global deflection of the solar wind by an intrinsic dipolar magnetic field, variations in solar wind momentum flux, and absence of such features as ionosphere, plasmasphere, and radiation belts, are described. Energetic electrons are accelerated in the magnetotail, however, and the interplanetary magnetic field variations distort Mercury's magnetosphere to produce a southward field associated with substorm-like disturbances.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: International Symposium on Solar-Terrestrial Physics; Jun 07, 1976 - Jun 18, 1976; Boulder, CO
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  • 45
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    Comparison of impact basins on Mercury, Mars and the moon (1976)
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    Publication Date: 2019-07-13
    Description: The statistics of basins on the moon, Mercury, and Mars are compared. The basic similarities of basins on Mars, Mercury, and the moon argue convincingly that they result from the same processes. Variations in onset diameters and relative abundances, however, suggest that these basic processes are modulated by second-order factors.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 46
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    Asteroids and comparative planetology (1976)
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    Description: The state of knowledge concerning the asteroids is reviewed and discussed in terms of the relationship of the asteroids with other solar system bodies. The data on spectral reflectances of asteroids are examined, and their implications for comparative planetology are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 47
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    Comparison of large crater and multiringed basin populations on Mars, Mercury, and the moon (1976)
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    Publication Date: 2019-07-13
    Description: The maximum regional areal densities of large impact craters on Mars, Mercury, and the moon appear to be inversely proportional to the surface areas of the planets. This would not be expected if the objects impacting the planetary surfaces came from common sources and were moving with high velocities relative to the planets; rather, a uniform areal density would be anticipated. Another way of stating the observation is that each planet was bombarded by the same number of objects. Two speculative explanations for the observation are that: (1) all planets underwent a uniform bombardment but were resurfaced by processes proportional to planetary surface area, or (2) equally populated families of objects, moving about the sun in orbits similar to those of the planets, were independently depopulated by the respective planets.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 48
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    Martian crater depth/diameter relationships - Comparison with the moon and Mercury (1976)
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    Publication Date: 2019-07-13
    Description: New Martian topographic data from Mariner 9 ultraviolet spectrometer (UVS) profiles provide depth data for 139 Martian craters of all degrees of degradation, between the diameters of 15 and 201 km. The population of Martian craters, including morphologically fresh examples, is shallower than both lunar and Mercurian fresh crater populations. Because the surface gravities of Mercury and Mars are identical within 5%, these differences in fresh crater depths suggest that factors other than gravity may play important roles in determining initial crater depths (e.g., differences in impact velocity, substrate variations, and Martian atmospheric effects during the crater-forming event). Degraded Martian craters are, on the average, no shallower than lunar pre-Imbrian craters of similar sizes. If the early bombardment of Mars was as significant a degradational agent as it was on the moon, then major levels of crater degradation and crater shallowing on Mars were associated with this mechanism. Continued eolian infilling, although locally significant, may be a less significant cause of morphometric degradation of large old Martian craters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 49
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    Carbonaceous chondritic xenoliths and planetary-type noble gases in gas-rich meteorites (1976)
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    Publication Date: 2019-07-13
    Description: The source of the planetary-type noble gases in gas-rich meteorites is identified as finely divided (submillimeter to millimeter-sized), widely dispersed carbonaceous chondritic fragments. Trace-element abundances, noble-gas elemental abundances and isotopic abundances of xenon are compatible with the hypothesis that the carbonaceous chondritic carrier is present in amounts of a few percent in the gas-bearing portions of gas-rich chondrites and achondrites.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 50
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    Shield volcanism and lithospheric structure beneath the Tharsis plateau, Mars (1976)
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    Publication Date: 2019-07-13
    Description: The heights of four great shield volcanoes, when interpreted as reflecting the local hydrostatic head on a common source of upwelling magma, provide significant constraints on models of lithospheric structure beneath the Tharsis plateau. If Bouguer gravity anomalies are modeled in terms of a variable thickness crust, and a two-component (crust/mantle) earth-like structure is assumed for the Martian lithosphere, the derived model lithosphere beneath the Tharsis plateau has the following properties: (1) the upper low-density 'crustal' component is thickened beneath the Tharsis plateau; (2) the lower high-density 'mantle' component is thinned beneath the Tharsis plateau; and (3) there is a net gradient on the base of the Martian lithosphere directed downward away from beneath the summit of the Tharsis plateau. A long history of magmatic intrusion is hypothesized to have been the cause of the updoming of the Tharsis plateau and the maintenance of the plateau in a state of only partial compensation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 51
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    Characterization of crust formation on a parent body of achondrites and the moon by pyroxene crystallography and chemistry (1976)
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    Description: Single crystal X-ray diffraction and electron microprobe techniques were used to study lunar crustal pyroxenes in a cataclastic norite, a pyroxene-rich clast, and anorthosite lunar samples, and also in meteorites including diogenites, eucrites, and the Yamoto (1) howardite. The crystallographic and chemical characteristics of pyroxenes in these materials are compared and are discussed in terms of the lower stability limit of pigeonite. A mechanical mixing model of howardite is proposed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 52
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    Thermal metamorphism of primitive meteorites. IV - Comparison with trends for ten trace elements in terrestrial basalt BCR-1 heated at 500-1000 C (1976)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 53
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    Chemical fractionation of Ru and Os in the moon (1976)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 54
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    Trace element evidence regarding a chondritic component in howardite meteorites (1976)
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    Publication Date: 2019-07-13
    Description: The concentrations of siderophiles Ni, Ge, Ru, Ir, and Au and volatiles Zn, Ga, Cd, and In in howardite meteorites were determined and are discussed along with similar data for eucrites and diogenites. The concentrations of the chondritic component in howardites are remarkably high. The concentrations in four high-siderophile howardites are comparable to those found in mature soils from the lunar highlands. The amounts of excess volatiles are roughly consistent with those expected if the chondritic component resemble CI, CM, or E4 chondrites. Evidence indicates that the howardite parent body had a radius of several hundred kilometers, and the most probable formation location was 1-2 AU from the sun.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 55
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    Convection cells in the early lunar magma ocean - Trace-element evidence (1976)
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    Publication Date: 2019-07-13
    Description: A method was proposed for recognizing suites of samples which are related to the differentiation of distinct and regionally separated magmas in the early lunar surface ocean. The sample suites were identified by three Cl-P2O5 compositional groups. New experimental data continue to add samples to these groups. Each magma was associated with a convection cell the boundaries of which are proposed. Independent geochemical evidence supporting a limited number of early magmas is cited. Two new possible Cl-P2O5 groups are identified. Samples not indigenous to a given site and their possible source regions are identified. It is proposed that many Apollo 17 basalts are not locally derived.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 56
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    Petrogenesis in a modestly endowed moon (1976)
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    Description: Four lines of recent evidence show that the moon is more modestly endowed in refractory elements and heat sources than previously thought. However, even this reduced endowment is adequate for the genesis of known lunar rock types. The thickness and nature of the initially molten zone and the structure of the crust and the lithosphere produced from it are the major uncertainties in models of lunar petrogenesis.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 57
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    Zr-Hf fractionation in chemically defined lunar rock groups (1976)
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    Publication Date: 2019-07-13
    Description: Zirconium and hafnium, a geochemically coherent pair of elements, are strongly fractionated in lunar rocks, as evidenced by a wide range of Zr/Hf mass ratios from 12 for the anorthosite 60015,65A to 50 for the KREEP breccia 14321. This may be explained in part by selective reduction of Zr(4+) to Zr(3+) and exclusion of the Zr(3+) from early crystallized Fe-Ti minerals.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 58
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    Limits for the accretion time of the earth from cosmogenic Ne-21 produced in planetesimals (1976)
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    Publication Date: 2019-07-13
    Description: Arguments are presented which show that no more than 23% of all neon-21 in the atmosphere consists of spallation Ne-21 formed by the bombardment of the earth's accreting objects by galactic cosmic rays. The amount of spallation Ne-21 depends strongly on the interpretation of the primitive, 'unirradiated' neon in the atmosphere. On the assumptions that (1) the planetesimals were irradiated by galactic cosmic rays of present-day intensity, (2) their mean lifetimes against accretion were 0.1 billion years, and (3) spallation Ne-21 was quantitatively retained by the accreting earth, and on the basis of Anders' (1965) reconstructed size distribution No. 2 of asteroids, the number of spallation Ne-21 atoms yielded amounts to 8.7% of the total number of Ne-21 atoms now on earth.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 59
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    On the global TRM of the lunar lithosphere (1976)
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    Publication Date: 2019-07-13
    Description: A global thermoremanent magnetization (TRM) theory is developed which takes into account the direction and magnitude of a hypothetical source dipole field, the distribution of magnetic permeability and the coefficient of TRM and the cooling rate in the lithosphere, and models the low-field TRM characteristics of the material. When applied to the moon in conjunction with lunar magnetic parameter ranges now available, the theory gives a permanent lunar dipole moment which is uncertain to a factor of about 10 to the 5th power.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 60
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    The geomagnetic dynamos of the moon and Venus - Comparisons with a recent scaling law (1976)
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    Publication Date: 2019-07-13
    Description: The evidence for the existence of an ancient lunar dynamo is reviewed along with the data on the magnetic field of Venus. These facts are then discussed in terms of Dolginov's scaling law for predicting magnetic moment of planets with a precession-driven dynamo. The precessional dynamo mechanism of Dolginov comes close to predicting the inferred magnetic moment of Venus, but this is viewed as a coincidence, for the Dolginov scaling law is based on an ad hoc force balance for which little justification is given. It assumes that the interiors of the planets have similar densities, conductivities, and precessional characteristics, whereas they clearly do not.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 61
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    Magnetic evidence concerning a lunar core (1976)
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    Publication Date: 2019-07-13
    Description: Two different methods were used to determine the lunar electromagnetic response: (1) comparison of Apollo 12 and Explorer 35 magnetometer data; and (2) observation of the dipole field configuration by orbiting Apollo 15 and 16 subsatellites. The methods give significantly different results. The subsatellite observations require the existence of a core, while the Apollo 12 and Explorer magnetometer measurements allow, but do not require, the existence of a core. Despite this, an upper limit of 580 km has been computed for the radius of the core.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 62
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    Magnetic effects of shock and their implications for lunar magnetism. II (1976)
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    Description: Synthetic breccias were produced by hypervelocity impact of projectiles on basalt powders in order to study the magnetization acquired during shock lithification of soil. It was found that some of the lithified products record the field at the point where they land, while others carry the original primary remanence. Even those rocks recording the direction of the ambient field did not always faithfully record the intensity of the field. When rocks were exposed to shock, it was found that the magnetic hardness of a rock has a profound effect on its magnetic response. Shock effects are seen at shock levels of less than 10 kbar, which suggests that lunar samples may have been shock-demagnetized.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 63
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    A solar origin for the large lunar magnetic field at 4.0 billion yr ago (1976)
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    Publication Date: 2019-07-13
    Description: A new method (Shaw, 1974) for paleointensity determination has been applied to three subsamples of one polymict breccia, 72215 (of age 4.0 billion yr) to yield an average paleointensity of 0.41 Oe at the Taurus-Littrow region of the moon around the time of breccia formation. Of the present models for lunar magnetism, only the Sonett and Runcorn (1974) model of a central iron core dynamo can explain the presence of such a large field in early lunar history. However, because of the similarity in size of this field and that for the early solar system deduced from carbonaceous chondrites, we draw attention to an apparently little-considered possibility: that the large magnetic field in early lunar history was external and solar in origin, and emanated from a pre-main sequence T-Tauri stage sun. Therefore, there should be no record of such a large magnetic field in lunar rocks younger than approximately 4.0 billion yr.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 64
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    Some complexities in the determination of lunar paleointensities (1976)
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    Publication Date: 2019-07-13
    Description: Application of a variant of the Thellier-Thellier method for paleomagnetic field intensity determination to an analog lunar sample revealed a peak at about 250 C on the partial thermoremanent magnetization (PTRM). Evidence suggests that this can be best explained by a partial self-reversal involving troilite becoming reversely magnetized in the presence of already magnetized intergrown iron. In lunar samples, an additional peak was observed. The results suggest that natural remanent magnetization of lunar samples is in part carried by interacting grains, so that paleointensity determinations on the basis of the assumption of noninteracting grains have to be discarded.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 65
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    Thermal expansion and thermal stress in the moon and terrestrial planets - Clues to early thermal history (1976)
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    Publication Date: 2019-07-13
    Description: The paper discusses how features of the surface geology of the moon and also Mars and Mercury impose constraints on the volumetric expansion or contraction of a planet and consequently provide a test of thermal history models. The moon has changed very little in volume over the last 3.8 b.y. Thermal models satisfying this constraint involve early heating and perhaps melting of the outer 200 km of the moon and an initially cold interior. Mercury has contracted by about 2 km in radius since emplacement of its present surface, so core formation must predate that surface. A hot initial temperature distribution is implied.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 66
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    Thermal diffusivity of four Apollo 17 rock samples (1976)
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    Description: The modified Angstrom technique was used to measure the thermal diffusivity of four Apollo 17 rock samples in air at pressures of 1 atm and one-millionth torr in the temperature range 80-460 K, and in CO2 at different pressures for various temperature ranges and at different temperatures for the range of interstitial CO2 gas pressure 1 atm to 0.0001 torr. The experiments with CO2 were intended to simulate Martian conditions, and it was found that the thermal diffusivity of lunar crystalline basalt and breccia varies very little with temperature in a simulated Martian environment, which indicates that the thermal processes in the Martian regolith could be more straightforward than in the lunar regolith.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 67
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    Filter processes applied to the scattering parts of lunar seismograms for identifying the 300 km discontinuity and the lunar grid system (1976)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 68
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    Revised lunar heat-flow values (1976)
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    Description: The 3.5- and 2-year subsurface temperature histories at the Apollo 15 and 17 heat-flow sites have been analyzed, and the results yield significantly lower thermal conductivity determinations than the results of previous short-term experiments. The thermal conductivity determined by probes at a depth of about 150 cm and 250 cm lies in the range 0.9-1.3 times 10 to the -4th W/cm K. On the basis of measurements of variations of surface thorium abundance and inferred crustal thicknesses, the average global heat flux is estimated to be about 1.8 microwatts/sq cm. This requires a uranium concentration of 46 ppb.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 69
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    Internal friction and velocity measurements (1976)
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    Description: The Q of a lunar basalt sample was measured under varying vacuum conditions, and it was found that even at pressures as low as 10 to the -7th to 10 to the -10th torr, substantial increases in Q with decreasing pressure are observed, while the resonant frequency increases only slightly. This suggests that only small amounts of volatiles are sufficient to increase the internal friction (lower the Q) dramatically. The technique of vibrating encapsulated samples in the torsional mode was used to measure Q of terrestrial rocks as a function of hydrostatic pressure under lunar vacuum conditions. Young's modulus measurements in the temperature range 25-600 C under a variety of conditions including high vacuum show no evidence of any irreversibility upon temperature cycling and no indication that the high Q-values obtained are associated with any permanent structure changes such as the formation of lossless 'welded' contacts.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 70
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    The asymmetric distribution of lunar maria and the earth's gravity (1976)
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    Description: The paper investigates the hypothesis that the asymmetry of the moon with respect to the distribution of maria, reflected in that the surface area of the moon covered by mare material is far greater on the earth-facing side than on the far side, is due to the action of the earth's gravity at a time when the moon was less distant from the earth than today. Such conditions would lead to gravitationally favored areas on the moon such that mare basalt magmas might erupt preferentially on the front side of the moon. Gravitational asymmetry is also discussed in terms of its effect on the shape of the moon, its center of mass, its moments of inertia, and the time scale for the evolution of its orbit.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 71
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    Seismic structure of the moon - A summary of current status (1976)
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    Description: A seismic model of the moon, refined from previous models with the aid of new data and analyses for seismic events recorded by four Apollo lunar seismic stations and a gravimeter, is outlined. The current model has five zones. The crust is 55-60 km thick. The surface is covered by regolith of varying thicknesses and low seismic velocity. The seismic Q's are extremely high. The upper mantle, 250 km thick, is characterized by seismic velocities close to those of the earth's upper mantle, and shear wave Q of about 4000. Tidally controlled deep moonquakes are concentrated near the boundary of the middle mantle, 600-700 km thick. A lower mantle extending to an undetermined depth is characterized by high attenuation of shear waves. The existence of a low-velocity core is only tentatively proposed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 72
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    Structure of the lunar interior from magnetic field measurements (1976)
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    Description: A network of lunar surface and orbiting magnetometers was used to obtain measurements of electrical conductivity and magnetic permeability of the lunar interior. An exceptionally large solar transient event, when the moon was in a geomagnetic tail lobe, enabled the most accurate lunar electromagnetic sounding information to date to be obtained. A new analytical technique using a network of two surface magnetometers and a satellite magnetometer superimposes many time series measurements to improve the signal-to-noise ratio and uses both the amplitude and phase information of all three vector components of the magnetic field data. Size constraints on a hypothetical highly conducting lunar core are investigated with the aid of the permeability results.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 73
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    Seismic investigation of the lunar interior (1976)
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    Description: The velocity and attenuation structure of the moon below the crust is examined using surface events. The moon is divided into an upper mantle and a lower mantle, the division at a depth of about 500 km being marked by a reflector identified on polarization filtered record sections. The upper mantle has a P-wave velocity of about 8 km/sec, a Poisson's ratio of about 0.25 and a Q for P waves of about 5000. This region contains no partial melt and is depleted in volatiles, notably water. The lower mantle has a lower S-wave velocity and probably a lower P-wave velocity than the upper mantle, with a Poisson's ratio of about 0.34. The lower mantle has a Q for P waves of approximately 1500, substantially lower than the upper mantle but probably still high enough to preclude partial melting. The velocity structure and the current value of the moment of inertia factor indicate an increase of density below about 500 km, perhaps due to an increase in iron content. We do not have any information directly pertaining to seismic velocities below 1000 km depth.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 74
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    High-explosive cratering analogs for bowl-shaped, central uplift, and multiring impact craters (1976)
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    Publication Date: 2019-07-13
    Description: The paper describes six experimental explosion craters in terms of their basic morphology, subsurface structural deformation, and surrounding ejecta blanket. These craters exhibit one or more of the following features: bowl shapes with underlying breccia lens, central uplifts, multirings, terraced walls, rim strata, zones of concentric rim deformation, inner continuous ground cover of ejecta blankets formed by overturned flaps, secondary cratering, and fused alluvium. These craters were formed by large shock wave energy transfers at or near zero heights-of-burst, and it is possible that impact craters with analogous morphologic and structural features may have formed under similar surface energy transfer conditions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 75
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    Impact ejecta on the moon (1976)
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    Description: The response of a lunar-sized object to the impact of meteoroids no more than about 100 km in radius is studied by means of a numerical model. The partitioning of impact energy into the kinetic and internal energy of the ejecta is obtained by using the conservation of mass, momentum, and energy conservation equations in finite-difference form within an Eulerian framework with approximate equations of state. The calculations are performed for a 15 km/sec impact of an iron object 5 cm in radius on a gabbroic anorthosite surface. Ejecta ballistic analysis is then performed. Most of the material lost escaping the moon is lunar crust material. Only 0.2% of the meteoroid escapes, all in the vapor phase.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 76
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    Candidate areas for in situ ancient lunar materials (1976)
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    Description: Results of high-speed impact cratering in quartz sand targets are reported. Dissection of the ejecta plumes of the craters revealed that they are relatively thin conical sheets. Further dissection showed the relationship between individual particle trajectories and the ejecta plume. A model of cratering, based on the experiments, was used to explain the inverted stratigraphy previously described in laboratory impact craters and in meteorite craters. Mantling of secondary craters in peripheral parts of the continuous deposits of Tycho Crater and in the downrange parts of certain Tycho secondary crater clusters is accounted for by the model. Model results indicate extensive mixing by secondary cratering when basin ejecta is emplaced. The study reveals certain areas on the lunar uplands that have been relatively uncratered by basin secondaries and unmantled by secondary crater debris surges and that may represent in situ ancient lunar materials.
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    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 77
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    The significance of substrate characteristics in determining morphology and morphometry of lunar craters (1976)
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    Description: Variations in the morphologic and morphometric characteristics of lunar craters appear to correlate well with the characteristics of the outer lunar crust and the presence of a 2-3 km thick megaregolith layer. These correlations suggest that substrate layering in general, and megaregolith in particular, may have an important effect on the excavation and modification stages in the formation of lunar craters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 78
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    Large scale cratering of the lunar highlands - Some Monte Carlo model considerations (1976)
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    Description: In an attempt to understand the scale and intensity of the moon's early, large scale meteoritic bombardment, a Monte Carlo computer model simulated the effects of all lunar craters greater than 800 m in diameter, for example, the number of times and depths specific fractions of the entire lunar surface were cratered. The model used observed crater size frequencies and crater-geometries compatible with the suggestions of Pike (1974) and Dence (1973); it simulated bombardment histories up to a factor of 10 more intense than those reflected by the present-day crater number density of the lunar highlands. For the present-day cratering record the model yields the following: approximately 25% of the entire lunar surface has not been cratered deeper than 100 m; 50% may have been cratered to 2-3 km depth; less than 5% of the surface has been cratered deeper than about 15 km. A typical highland site has suffered 1-2 impacts. Corresponding values for more intense bombardment histories are also presented, though it must remain uncertain what the absolute intensity of the moon's early meteorite bombardment was.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 79
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    Photogeology of the multi-ringed crater Haldane in Mare Smythii (1976)
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    Description: Haldane is a 40 km multi-ringed crater that occurs along with similar structures in a belt within the Smythii Basin. It is the best developed structurally of all craters in this belt and displays examples of all materials units of Mare Smythii. In addition to the outer rim, the crater displays a sharp-crested, nearly complete inner ring, and a complex central peak of round hills that are 300-600 m higher than the floor. There are two fracture systems associated with Haldane, one annular and the other radial. The annular fractures seem to control the deposition of mare basalts and dark mantle units in and around the crater. Topographic evidence and flow scarps indicate that the crater was the source of mare basalts and associated dark mantle, rather than its being flooded by such deposits. There are numerous indications that most of the features in and around Haldane are attributable to volcano-tectonic modifications of an original crater-form.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 80
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    Secondary impact craters of lunar basins (1976)
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    Description: Numerous lunar features are examined and identified as being secondary to basins, that is, as having been formed by secondary impact of ejecta from basins. Most of the terra features previously attributed to volcanism and tectonism and many attributed previously to primary impact must be attributed to basin-secondary impact. Secondary craters of the Imbrium Basin cover a large part of the south-central near side. Imbrium secondaries are more numerous than primaries in the size ranges 3 or 4 to 10 km on the near side, and may be more numerous at diameters of 10-25 km. Preliminary stratigraphic dating results based on superposition relations among basin secondaries suggest that the Crisium and south Serenitatis basins are younger than Nectaris and Humboldtianum.
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    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 81
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    Multiple ring structures and the problem of correlation between lunar basins (1976)
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    Description: Comparison of multi-ringed, mare-filled basins on the nearside of the moon indicates that a simple one-to-one correspondence of all rings between lunar basins does not exist. The only rings which can be correlated reasonably well between such basins are concentric systems of mare ridges and basin rims, and the frequently cited square-root-of-2 spacing relationship does not correctly describe their spacing. It is concluded that the Cordillera is the rim of the Orientale Basin and is equivalent to the 1340 km diameter ring of the Imbrium Basin and the rims of the other mare-filled basins. The area between the Rook and Cordillera rings is believed equivalent to the marginal shelf areas of the more completely mare-filled basins. A circular arc approximately 520 km diameter located just inside the outer Rook Ring would have been the most likely site for formation of a concentric system of mare ridges, had filling of the Orientale Basin been complete.
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    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 82
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    The scarcity of mappable flow lobes on the lunar maria - Unique morphology of the Imbrium flows (1976)
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    Description: Unique features of Imbrium lava flows are their thickness (10-30 + m) and lengths (up to 400 km for phase-III, and up to 600 km for phase-II) when compared along later Imbrium and Eratosthenian units. They are distinct by virtue of their inferred short-lived (on the order of days) and extremely rapid rates of effusion. It is shown that there are numerous other basalt eruptives within the young blue western maria. The emplacement of these flows was by complex multilayering and intertonguing of individual flow units with thicknesses less than 10 m. They are generally restricted to the near vicinity of multiple vent sources.
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    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 83
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    The morphological evolution of mare-highland contacts - A potential measure of relative mare surface age (1976)
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    Description: The uniform breaks in slopes along many mare-highland contacts may be debris aprons transported primarily by impact erosion at relatively slow rates. Other suggestions, such as the 'high lava mark' hypothesis, appear inadequate to explain all of the unique characteristics of these widespread features. There is a reasonable correlation of overall slope form (profile) and apron distribution with established mare age provinces. Distinctive debris aprons in the younger maria could represent the initial stages of lunar slope degradation produced mainly by the postmare impact flux. The growth of debris aprons must be qualitatively related to the impact flux recorded on adjacent mare surfaces and could provide an approximate means of extrapolating relative mare ages to highland scarps and crater walls. By combining detailed measurements of lunar slopes with development of a realistic model for impact modification of these features, approximate limits for the cumulative lunar flux distribution through time might be derived.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 84
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    Cosmic ray exposure ages of Apollo 17 samples and the age of Tycho (1976)
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    Description: Cosmic ray exposure data for Apollo 17 samples and quantitative photogeologic data are presented which support the hypothesis that the Central Cluster unit and the Bright Mantle at the Apollo 17 landing site are related to impact of ejecta from the crater Tycho, lying about 2000 km to the southwest. The exposure ages point to a site-wide event 96 m.y ago, which included emplacement of the Bright Mantle and Central Cluster units.
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    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 85
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    Modes of emplacement of basalt terrains and an analysis of mare volcanism in the Orientale Basin (1976)
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    Publication Date: 2019-07-13
    Description: Three distinctive types of basalt terrains can be recognized on earth on the basis of surface morphology: flood basalts, shield basalts, and plains basalts, each of which reflects unique styles of eruption and modes of emplacement. Two of these, flood basalts and plains basalts, appear to be important in the emplacement of mare basalts on the moon. Using surface features as identifying criteria, mare units in the Orientale Basin were examined and the following emplacement sequence was derived: (1) initial emplacement of impact melt in the basin center, (2) eruption of flood-type basalts in the basin center and approximately concurrent emplacement of plains type basalts in Lacus Veris, and (3) emplacement of plains type basalts in Lacus Autumni
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 86
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    Geologic structure of the eastern mare basins (1976)
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    Publication Date: 2019-07-13
    Description: The thickness of mare basalts in the eastern maria are estimated and isopachs of the basalts are constructed. Sub-basalt basin floor topography is determined, and correlations of topographic variations of the surface with variations in basalt thickness or basin floor topography are investigated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 87
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    Mare ridges and related highland scarps - Result of vertical tectonism (1976)
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    Publication Date: 2019-07-13
    Description: Two fresh-looking scarps on the rim of the Serenitatis Basin were structurally analyzed in detail on high-resolution stereoscopic photographs. The scarps are topped by wrinkle ridges on the mare and transgress into adjacent highlands. They are faults that offset mare and highland surfaces. The faults appear to have high-angle fault planes and both normal and reverse separation which suggests tensional as well as compressional stresses. These observations, though contradictory in regional stress systems, are compatible with local adjustments resulting from vertical tectonic movement. A model is developed that fits the observations and proposes that ridges and scarps formed through vertical structural adjustment caused by gravitational settling, and following older structural trends.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 88
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    Ages of flow units in the lunar nearside maria based on Lunar Orbiter IV photographs (1976)
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    Publication Date: 2019-07-13
    Description: A map dividing the lunar nearside maria into six units each of uniform age was compiled from Lunar Orbiter IV photographs. Relative ages were determined using a crater morphology technique. Relative ages were then converted to absolute ages by comparison to a curve calibrated from Apollo and Luna sample data; three of the six units, including the two youngest (about 3.1 and 2.6 b.y. old), were not sampled by Apollo or Luna. Vast regions in the western maria are covered by these young flows. The old flows (about 3.75 b.y. in age) are found to occur mostly in the eastern maria. A comparison of the age units derived from these data with those units derived from other remote-sensing data provide good agreement in the location of unit boundaries. These data also indicate that the emplacement history of mare basalt types is more complex than was earlier thought.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 89
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    Degradation of large, period II lunar craters (1976)
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    Publication Date: 2019-07-13
    Description: Nighttime thermal maps of large, young lunar craters show an evolutionary sequence in the gross morphology of thermal patterns associated with the craters. The nature of the sequence is consistent with crater degradation models which predict a filling of large craters with material from the walls. Detailed comparison of a nighttime thermal map of Copernicus with a geologic map demonstrates that a smooth floor unit characterized as impact melt is more likely wall debris. Nighttime thermal maps will be particularly useful for quantifying crater modification which has occurred in the relatively quiescent post-basin period of lunar history.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 90
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    Characterization of lunar mare basalt types. I - A remote sensing study using reflection spectroscopy of surface soils (1976)
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    Publication Date: 2019-07-13
    Description: Telescopic reflection spectra of mature mare surfaces are used to identify and characterize major basalt types on the frontside of the moon. The spectra are classified according to (1) continuum slope and (2) near-infrared features. This study indicates that there are major lunar basalt types that are unlikely to have been sampled during the landing missions. Regions of basalt exist in the western maria with a TiO2 content comparable to that of Apollo 11 but with infrared characteristics that indicate a distinctly different composition. Samples from two landing sites, Apollo 12 and Luna 16, may contain fragments of a nearby basalt unit compositionally different from the dominant basalt type of the landing area.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 91
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    Surface chemistry of selected lunar regions (1976)
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    Publication Date: 2019-07-13
    Description: A completely new analysis has been carried out on the data from the Apollo 15 and 16 gamma-ray spectrometer experiments. The components of the continuum background have been estimated. The elements Th, K, Fe, and Mg give useful results; for Ti are significant only for a few high-Ti regions. Errors are given, and the results are checked by other methods. Concentrations are reported for about 60 lunar regions; the ground track has been subdivided in various ways. The borders of the maria seem well-defined chemically, while the distribution of KREEP is broad. This wide distribution requires emplacement of KREEP before the era of mare formation. Its high concentration in western mare soils seems to require major vertical mixing.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 92
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    Lunar surface remanent magnetic fields detected by the electron reflection method (1976)
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    Publication Date: 2019-07-13
    Description: We present maps of the lunar surface remanent magnetic fields detected by the electron reflection method. These maps provide substantial coverage of the latitude band from 30 N southward to 30 S with a resolution of about 40 km and a sensitivity of about 0.2 gamma at the lunar surface. Regions of remanent magnetization are observed ranging in size from the resolution limit of 1.25 deg to above approximately 60 deg. The largest contiguous region fills the Big Backside Basin where it is intersected by the spacecraft orbital tracks. Preliminary analyses of the maps show that the source regions of lunar limb compressions correspond to regions of strong surface magnetism, and that there does not appear to be sharply discontinuous magnetization at the edges of maria. We also analyze the electron reflection observations to obtain information on the direction and distribution of magnetization in the Van de Graaff anomaly region.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 93
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    A geochemical anomaly contiguous with the Dorsa Geike wrinkle ridge in Mare Fecunditatis (1976)
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    Publication Date: 2019-07-13
    Description: The orbital Al/Si X-ray fluorescence data from Apollo 15 and 16 reveal a concentration of unusually low Al/Si intensity ratios associated with a 220-km long ray along the northeast-southwest trending wrinkle ridge, Dorsa Geike, of the Mare Fecunditatis. The paper describes in detail the analysis of the Al/Si X-ray fluorescence data by which this geochemical anomaly was discovered. Correlation with other remote sensing data also indicates that the ridge area is different from the rest of the mare. It is possible that the material associated with the low Al/Si intensity ratio is of different composition than the adjacent mare regolith. Downslope transport along the ridge and arch could expose basalts which contrast chemically with surrounding regolith. The anomaly could also be due to extrusion of a volcanic rock of different composition at the fracture system represented by the wrinkle ridge.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 94
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    Quantitative mass distribution models for Mare Orientale (1976)
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    Publication Date: 2019-07-13
    Description: Six theoretical models for the mass distribution of Mare Orientale were tested using five gravity profiles extracted from radio-tracking data of orbiting spacecraft. The models with surface mass and moho relief produced the best results. Although there is a mascon-type anomaly in the central maria region, Mare Orientale is a large negative gravity anomaly. This is produced primarily by the empty ring basin. Had the basin filled with maria material it seems likely that it would have produced a mascon such as those presently existing in flooded frontside circular basins.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 95
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    Electrical properties of Apollo 17 rock and soil samples and a summary of the electrical properties of lunar material at 450 MHz frequency (1976)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 96
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    Lunar farside gravity - An assessment of satellite to satellite tracking techniques and gravity gradiometry (1976)
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    Publication Date: 2019-07-13
    Description: The estimation of local gravity anomalies represented by point masses using gravity gradiometer and satellite to satellite tracking data is discussed. A simulation analysis has been performed to study the recovery of local gravity anomalies from both rotating single axis gravity gradiometer and satellite to satellite tracking measurements. A Lunar Polar Orbiter mission concept is adopted for the orbits and data links. The sensitivity of the gravity determination to data noise, mass point spatial distribution (model errors), unmodelled gravity (gravity anomalies outside the area of interest), and orbit errors is studied. Figure of merit for the comparison is the rms error of radial acceleration.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 97
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    Age-color relationships in the lunar highlands (1976)
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    Publication Date: 2019-07-13
    Description: The depth of the absorption feature near 1 micron in the reflectance spectra of immature lunar soils is determined primarily by the amount of pyroxene present in the soil. As a soil matures, the agglutinitic glass content increases and the Fe(2+) glass band dominates the absorption feature. An empirical relationship between the 1 micron band depth and the percentage of magnetic agglutinates, and hence maturity, is demonstrated for mature highland soils of a given composition. A similar variation of 1 micron band depth is observed in the telescopic spectra of lunar highland craters and is positively correlated with the surface maturity as determined by the small-impact erosion model of Soderblom (1970). Knowledge of both maturity and the 1 micron band depth of a lunar surface feature allows compositional information to be derived.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 98
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    Crystallization kinetics, viscous flow, and thermal histories of lunar breccias 15286 and 15498 (1976)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 99
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    Further characterization of spectral features attributable to titanium on the moon (1976)
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    Publication Date: 2019-07-13
    Description: The following transitions are observed in the electronic absorption spectra of lunar titanaugites: Fe(2+) spin-allowed and spin-forbidden crystal field; Ti(3+) spin allowed and Jahn-Teller split crystal field; Ti(3+)-Ti(4+) CT; Fe(2+)-Ti(4+) CT; and O(2-)-Fe(2+), Ti(3+), Ti(4+) CT. Of these, the transitions involving Ti(3+) are unique to lunar or nonferric-bearing titanaugites. All titanaugites have the Fe(2+) crystal field and Fe(2+)-Ti(4+) CT transitions in common. These features in the diffuse reflectance spectra of lunar materials give rise to the '1.0 band' and to the observed absorption around 0.5-0.6 micron, respectively. Since regolith contains a variety of phases with coexisting Fe(2+), Ti(3+), and Ti(4+) ions, several metal-metal charge transfer processes are possible.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 100
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    Thermal model for impact breccia lithification - Manicouagan and the moon (1976)
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    Publication Date: 2019-07-13
    Description: The thermal model of Simonds (1975) is extended to the full spectrum of impact-produced rocks ranging from fragmental breccias to impact melts, with reference to the Manicouagan impact structure in Quebec. This is done by relating the basic textural features of impact-lithified rocks to variations in the mixture of superheated impact-fused material originating near the point of impact and much cooler fragmented debris originating farther from the point of impact.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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