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  • LUNAR AND PLANETARY EXPLORATION  (815)
  • Animals  (374)
  • 1995-1999
  • 1985-1989
  • 1975-1979  (1,189)
  • 1979  (1,189)
Collection
Keywords
Publisher
Years
  • 1995-1999
  • 1985-1989
  • 1975-1979  (1,189)
Year
  • 1
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    Aeronautics and Space Highlights [1979 Highlights] (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: The videotape includes footage of the following: Voyagers to Jupiter, Pioneer to Saturn, High Energy Astronomy Observatory, space telescope, space shuttle, astronauts Young and Crippen, 10th anniversary of Apollo 11, Skylab reentry, Landsat, satellite freeze warning, Fire Fighting Module, SAGE, wind generators, Solar Energy Project, electric car research, XV-15, HiMAT, and crash worthiness tests.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: ASR-178 , NASA-TM-109443 , NONP-NASA-VT-93-190240
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  • 2
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    Mass spectrometry measurements of the lower atmosphere of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Mass spectrometer experiments installed on the descent vehicles of the Venera-11 and the Venera-12 are described. Data on the chemical composition of the lower atmosphere of Venus is discussed with emphasis on the isotope state of the basic components (carbon, oxygen, nitrogen) and of the inert gases.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75477
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  • 3
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    An Analysis of the Chemical Composition of the Atmosphere of Venus on an AMS of the Venera-12 Using a Gas Chromatograph (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Eight analyses of the atmosphere of Venus were made beginning at an altitude of 42 km right down to the surface of the planet. The following were detected in the atmosphere of Venus: nitrogen in concentrations of 2.5 plus or minus 0.5 volumetric %, argon ir concentrations (4 plus or minus 2) x 10 to the minus 3 power volumetric %, CO--(2.8 plus or minus 1.4) x 10 to the minus 3 power volumetric % and SO2 in concentrations (1.3 plus or minus 0.6) x 10 to the minus 2 power volumetric %. The upper limits were estimated for the content of oxygen and water equal to 2 x 10 to the minus 3 power and 10 to the minus 2 power volumetric %, respectively.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75476
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  • 4
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    Voyager 2 Jupiter encounter (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: A NASA News Release is presented which contains the following: (1) general release; (2) two views of Voyager 2 flight past Jupiter; (3) Voyager mission summary; (4) Voyager 1 science results; (5) Jupiter science objectives; (6) Jupiter the planet and its satellites; (7) Voyager experiments; (8) planet comparison; (9) a list of Voyager science investigators and (10) the Voyager team.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-79-86 , P79-10088
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  • 5
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    Altitude-age relationships of the lunar maria (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: Altitudes and relative ages of mare surface units were compared to test if a systematic correlation in height of lava eruption surfaces and age might reflect a corresponding increase in depth of the magma chamber with time; in addition the altitudes were studied to shed light on the time and place of warping of mare surfaces. The laser altimeter data from the Apollo missions and relative age data based on crater erosion models and crater counts were used for the study. The data were correlated by using the image data bank of the Lunar Geoscience Consortium. Results of the first part of the study are inconclusive as no systematic increase in height of lavas with time could be shown. The data of the second part of the study support the conclusion that mare surfaces may have warped throughout most of the time represented by sample ages from the Apollo missions, and that the lithosphere may have become strong enough to remain stable after the time of Apollo 12 samples around 3 b.y. ago.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 6
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    On the structure of the upper atmosphere of Mars according to data from experiments on the Viking space vehicles (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Altitude profiles of the concentrations of the atmospheric components measured by the on board mass spectrometers during the descent of Viking lander are discussed by assuming that temperature has a smoother profile, and the eddy mixing coefficients are smaller at altitudes of 120 to 170 km than those formally determined. The influence of acoustic gravitational waves and errors in measurements and calculations are discussed in relation to the convolutions in the altitude profiles of the concentrations of the atmospheric components and the temperature of the atmosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75717 , PR-343
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  • 7
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    Dynamics of the accumulation process of the Earth group of planets: Formation of the reverse rotation of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: A numerical simulation of the process of formation of the terrestrial planets is carried within the framework of a new theory for the accumulation of planetary and satellite systems. The numerical simulation permitted determining the parameters of the protoplanetary disk from which Mercury, Venus and the Earth were formed as result of the evolution. The acquisition of a slow retrograde rotation for Venus was discovered during the course of the investigation, whereas Mercury and the Earth acquired direct rotation about their axes. Deviations of the semimajor axes of these three planets as well as the masses of the Earth and Venus from the true values are small as a rule (l 10%). It is shown that during the accumulation of the terrestrial planets, there existed a profound relationship between the process of formation of the orbits and masses of the planet and the process of formation of their rotation about their axes. Estimates are presented for the radii of the initial effective bodies and the time of evolution for the terrestrial accumulation zone.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75641 , PREPRINT-135
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  • 8
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    Report of the Comet Science Working Group (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Scientific objectives and mission strategies for a flyby of Halley's comet and rendezvous with Tempel-2 are discussed. Instrumentation to be carried by both the rendezvous spacecraft and the coma probe payload are listed. Known characteristics of both comets are summarized.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-80542
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  • 9
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    The Planet Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Physical features of the planet Venus, including its rotational characteristics and the surface properties observed by NASA's Deep Space Network radar scanner and Soviet spacecraft are examined. Atmospheric composition and circulation and the nature of the Venus clouds are also discussed in this instructional pamphlet. A reading list and student projects are included.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-79954 , NF-86/12-77
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  • 10
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    Report of the Comet Science Working Group (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: General scientific questions and measurement objectives that can be addressed on a first comet mission relate to: (1) the chemical nature and the physical structure of comet nuclei as well as the changes that occur as functions of time and orbital position; (2) the chemical and physical nature of the atmospheres and ionospheres of comets, the processes which occur in them, and the development of these atmospheres and ionospheres as functions of time and orbital position; and (3) the nature of comet tails, the processes by which they are formed, and the interaction of comets with the solar wind. Capabilities of the various instruments required are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-80543
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  • 11
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    Voyager 1 examines Jupiter (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: An overview of the Voyager mission to Jupiter, Saturn, and possibly Uranus is presented. Scientific instruments onboard the spacecraft are described as well as methods used for their calibration and evaluation during the cruise phase of the mission. Experiments to be performed cover the following areas: imaging science, radio science, cosmic rays, ultraviolet spectroscopy, photopolarimetry, planetary radio astronomy, magnetic fields, low-energy charged particles, plasma science, and infrared radiometry and spectroscopy. A list of the satellites of Jupiter and their diameters, distances, and periods is included.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-79-23 , P79-10024
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  • 12
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    Viking Orbiter imaging observations of dust in the Martian atmosphere (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: More than 20 local Martian dust clouds and two global dust storms were observed with the Viking Orbiter camera. Sixteen of the local clouds were imaged in two colors or were observed with other instruments confirming their identification as dust clouds. These Viking results are compared with earth-based observations of Martian dust storms and with Mariner 9 data. Most of the dust activity seen by Viking occurred during southern hemisphere spring and early summer, when Mars was near perihelion and insolation was near maximum. About half the local clouds occurred near the edge of the southern polar cap, where winds are presumably enhanced by a strong regional temperature gradient. The other half occurred mainly in the southern hemisphere near regions where circulation models incorporating topography predict positive vertical velocities. Although dust clouds observed from earth show a similar partial correlation with models, some ambiguity exists concerning interpretation of regions near Hellespontus that have spawned the most spectacular Martian dust storms on record.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 84; June 10
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  • 13
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    Seasonal recession of Mars' south polar cap as seen by Viking (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: The spring-summer retreat of the south polar cap of Mars is portrayed in photomosaics obtained by Viking Orbiter 2 during 1977. Comparisons of these data to Mariner 9 photos and to the record of telescopic observations attest that the polar retreat viewed by Viking was significantly slower than those previously reported. A global dust storm which occurred at an unusually early season may have effected this retarded recession by introducing dust into the atmosphere of Mars which modified the polar energy balance through scattering of incident radiation. The composition of the south residual cap cannot be unambiguously determined at this time; however, some data suggest that CO2 or clathrate survived the entire summer viewed by Viking.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 84; June 10
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  • 14
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    Viking observations of a Martian climate fluctuation (1979)
    In:  Other Sources
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    Publication Date: 2019-08-28
    Description: The retreat of Mars' south polar cap during spring and summer was observed in detail by Viking orbiters. This regression was significantly slower than those observed previously by telescope and by Mariner 9. The retardation may have been caused by a reduction in surface insolation brought about by aerosols produced in an unusually early global dust storm.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: In: Evolution of planetary atmospheres and climatology of the earth; International Conference; Oct 16, 1978 - Oct 20, 1978; Nice; France
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  • 15
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    Electrical discharges in the atmosphere of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Data received from Venera 11 and 12 experiments involving the electrical activity of the atmosphere of Venus show that the electrical discharges occur in the cloud layer. Their energy is roughly the same as in terrestrial lightning, but with a pulse repetition frequency of the discharges which is much greater.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75639
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  • 16
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    NASA Facts: an Educational Publication of the National Aeronautics and Space Administration. the Voyager Mission (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: The evolution of Jupiter, as well as its rotation, atmosphere and magnetosphere are described in this third in a series of publications on the exploration of the outer planets by the Voyager spacecraft. Activities for student participation are included with a selected reading list.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-79953 , NF-89
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  • 17
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    Standard techniques for presentation and analysis of crater size-frequency data (1979)
    In:  Other Sources
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    Publication Date: 2019-08-27
    Description: In September 1977 a crater studies workshop was held for the purpose of developing standardized data analysis and presentation techniques. The present report contains the unanimous recommendations of the participants. Recommendations are devoted primarily to crater size-frequency data and refer to cumulative and relative size-frequency distribution plots and to morphological analysis.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 37; Feb. 197
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  • 18
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    Voyager program. Voyager 1 encounter at Jupiter, 5 March 1979 (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: Highlights of Voyager 1 activity during the observatory and far-encounter phases are summarized. Daily sequence of events for the spacecraft during the period of greatest encounter activity (Feb. 26 through Mar. 7) the near-encounter phase is given. Times shown designate the time of signal reception at Deep Space Network stations. Events listed emphasize activities pertaining to the four remote sensing instruments on the scan platforms. However, the other 7 experiments will continuously collect data throughout the encounter period.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-79993 , S-802-77-01/02
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  • 19
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    The Galilean satellites and Jupiter - Voyager 2 imaging science results (1979)
    In:  Other Sources
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    Publication Date: 2019-08-27
    Description: Continuous global observations of Jupiter were made by Voyager 2 for a period of 63 days. Voyager 2 provided images that both complement and supplement the Voyager 1 images. The combined Voyager 1 and 2 observations of Jupiter provide an almost continuous record, over a 6-month period, of the behavior of the Jovian atmosphere at a resolution far better than can be obtained from earth-based studies. The present report briefly describes the changes in the cloud morphologies and local atmospheric motions. On Io, changes are observed in eruptive activity, plume structure, and surface albedo patterns. Europa's surface retains little or no record of intense meteorite bombardment, but reveals a system of overlapping bright and dark linear features. Ganymede exhibits at least one unit of heavily cratered terrain on a surface that otherwise suggests widespread tectonism. Except for two large ringed basins, Callisto's entire surface is heavily cratered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science; 206; Nov. 23
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  • 20
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    Venera-11 and Venera 12: Preliminary estimates for the wind speed and turbulence in the atmosphere of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: The methods and results of measurements for wind speed and atmospheric turbulence in the clouds of Venus are described, and compared with earlier results. The distribution of wind speed obtained from the data of Venera 12 is in good conformity with the data of the preceding Venera and Pioneer probes, indicating the existence of a constant and powerful zonal movement of the troposphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75726
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  • 21
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    Voyager pictures reveal new moon of jupiter (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-79-132 , P-79-10130
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  • 22
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    Numerical modelling of the formation process of planets from protoplanetary cloud (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: Evolution of the plane protoplanetary cloud, consisting of a great number of gravitationally interacting and uniting under collision bodies (protoplanets) moving in the central field of a large mass (the Sun or a planet), is considered. It is shown that in the course of protoplanetary cloud evolution the ring zones of matter expansion and compression occur with the subsequent development leading to formation of planets, rotating about their axes mainly directly. The principal numerical results were obtained through digital simulation of planetary accumulation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75642 , PREPRINT-134
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  • 23
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    Results and interpretation of measurements of the light flux in the near-surface layer of the Venusian atmosphere (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: The characteristics of the field of radiation in the near surface layer of the atmosphere and on the surface of Venus are reported. Optical measurements made during the landing of the descent vehicles are described. The relief of the surface and the amount of dust on it are examined. The spectral relationship of the albedo of the soil and the light flux incident on the surface is discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75716 , PR-338
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  • 24
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    Tectonics and volcanisms of Mars (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: Televised images of Mars transmitted from interplanetary stations are used to develop a theory of the structure and development of the planet. Crater chronology, the structure of planetary bodies in the Earth group, and a comparison of the Earth planetary bodies are among the factors included.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75604
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  • 25
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    Second International Colloquium on Mars: Abstracts for a colloquium (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-27
    Description: Abstracts of 110 papers relating to investigations of the planet Mars and intended for consideration at the colloquium are presented. Entries are arranged alphabetically according to the author's name.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CP-2072 , Jan 15, 1979 - Jan 18, 1979; Pasadena, CA; United States
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  • 26
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    Galileo to Jupiter: Probing the Planet and Mapping Its Moons (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: The first project to use the space shuttle as an interplanetary launch vehicle, the Galileo mission is designed to obtain information about the origin and evolution of the solar system by studying large-scale phenomena on Jupiter and its satellites. Aimed towards Mars to obtain gravity assist, the orbiting spacecraft will deploy a probe, which penetrating the Jovian atmosphere, will transmit data for approximately an hour. The spacecraft itself will inspect the atmospheres, ionospheres, and surfaces of Ganymede, Io, Europa, and Callisto, as well as determine their magnetic and gravitational properties. The experiments to be conducted and their scientific objectives are described. Known facts about the Jovian system are reviewed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-162142 , JPL-400-15-7/79
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  • 27
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    The structure and microphysical properties of the clouds of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-13
    Description: Results are presented from the processing and interpretation of measurement data in the descent capsules of the automatic stations Venera-9 and Venera-10 for the characteristics of light scattering in the atmosphere of Venus by means of onboard nephelometers. A model for the aerosol component in the planet's atmosphere in the altitude range 62-14 km is proposed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75725 , PREPRINT-144
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  • 28
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    Early findings from Pioneer Venus (1979)
    In:  CASI
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    Publication Date: 2019-08-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-79-13 , P79-10013
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  • 29
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    Viking cameras reveal new Martian frost layer (1979)
    In:  CASI
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    Publication Date: 2019-08-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-NEWS-RELEASE-79-107 , P79-10107
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  • 30
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    Spectrophotometric experiment on the Verera-11 and Venera-12 descent vehicles: Some results of the analysis of the spectrum of the daytime sky of Venus (1979)
    In:  CASI
    Details
    Publication Date: 2019-08-13
    Description: The spectra of the daytime sky of Venus were recorded on the Venera-11 and Venera-12 descent vehicles at various altitudes above the planet's surface, within the interval of 4500 to 12,000 Angstroms. The angular distribution of the brightness of the scattered radiation was recorded and the ratio of water and carbon dioxide were studied, with respect to the cloud cover boundaries.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-75640
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  • 31
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    The Pioneer Venus Missions (1979)
    In:  Other Sources
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    Publication Date: 2019-07-27
    Description: Two spacecraft with scientific instruments, a Multiprobe and an Orbiter, were sent to Venus by the USA in 1978 and successfully performed a series of measurements of the Venusian environment, in situ from the probes and remotely from the Orbiter. The paper discusses the scientific objectives of the missions, describes the spacecraft and trajectories, presents the performance of the spacecraft and instruments, and summarizes the scientific findings. The results indicate an excess of primordial argon at Venus; four distinct cloud layers were observed; four widely separated sites in both daylight and night time show almost no differences in atmospheric temperature and pressure below about 50 km altitude; winds up to 200 m/sec were observed at high altitudes; large plateaus were identified on the surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: IAF PAPER 79-147 , International Astronautical Federation, International Astronautical Congress; Sept. 17-22, 1979; Munich
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  • 32
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    The effects of ultraviolet light on the degradation of organic compounds - A possible explanation for the absence of organic matter on Mars (1979)
    In:  Other Sources
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    Publication Date: 2019-07-27
    Description: The analysis of the top layer of the Martian regolith at the two Viking landing sites did not reveal any indigenous organic compounds. However, the existence of such compounds at deeper layers cannot be ruled out. Cosmochemical considerations indicate various potential sources for organic matter on Mars, such as comets and meteorites. The study tested the stability of a sample of the Murchison meteorite and various organic substances which have been detected in carbonaceous chondrites, such as glycine, adenine and naphthalene, to the action of ultraviolet light. The compounds were adsorbed on powdered quartz and on California desert soil and were irradiated in the presence or absence of oxygen. The organic content, before and after irradiation, was measured by carbon elementary analysis, UV-absorption, amino acid analysis or pyrolysis-gas chromatography-mass spectrometry. In the absence of oxygen, adenine and glycine appear to be stable over the given part of irradiation. A definite degradation was noticed in the case of naphtalene and the Murchison meteorite. In the presence of oxygen in amounts comparable to those on Mars all compounds were degraded. The degree of degradation was influenced by the irradiation time, temperature and oxygen content.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 33
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    The Viking results - The case for man on Mars (1979)
    In:  Other Sources
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    Publication Date: 2019-07-27
    Description: The Viking landers have provided a number of insights into the composition of the Martian atmosphere and soils (e.g. the high Ar-40/Ar-36 ratio in the atmosphere, and the very low level of organic molecules in the Martian soil). However, a manned mission to Mars could yield much needed additional information on the planet. Seismic and electromagnetic sounding surveys, cloud tracking, drilling for permafrost, and the deduction of geologic field relationships are among the tasks for which a manned research endeavor is particularly suited. Rocket propellant synthesis and the production of food on Mars may be necessary to support such a manned mission.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: AAS 78-156
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  • 34
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    Photogeological constraints on lunar and planetary vulcanism, part 1 (1979)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: Central volcanic constructs were studied as constraints on the thermal evolution and regional tectonics of the Moon and terrestrial planets. The origins of sub-kilometer lunar craters were examined with regards to implications for mare basalt petrogenesis. The morphology, distribution, age, and tectonic setting of the volcanic constructs were studied using Viking Orbiter data.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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    Geologic problems in the northern plains of Mars (1979)
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    Publication Date: 2019-07-13
    Description: Viking pictures have made it possible to subdivide the few broad plains categories recognized on Mariner-9 pictures into smaller more definitive geologic units. Mapping problems arise in places where image resolution is sufficient to reveal the texture characteristics of individual units, but does not disclose the nature of their boundaries nor their stratigraphic relations. The mottled plains remain the most extensive undivided geologic unit in the northern Martian hemisphere; they may represent the northern remnant of the highlands, separated by crustal extension. Further resolution of the mottled plains unit may depend largely on digital enhancement of pictures in selected areas.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Origin of Valles Marineris (1979)
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    Publication Date: 2019-07-13
    Description: The purpose of the paper is to propose an origin of Valles Marineris and contiguous features such as Noctis Labyrinthus, chaotic terrain, and the large channels of Mars. These are found to: (1) be continuous to each other, (2) have gradual transition between the morphologies, (3) be related by tectonic fracturing, and associated with features of possible magmatic origin. A model is presented in which the geological process is a magmatic process, and after initial uplift and fracturing, Valles Marineris, Noctis Labyrinthus and some chaotic terrain were produced by subsidence caused by lava withdrawal.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Martian soil stratigraphy and rock coatings observed in color-enhanced Viking Lander images (1979)
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    Publication Date: 2019-07-13
    Description: Subtle color variations of martian surface materials were enhanced in eight Viking Lander (VL) color images. Well-defined soil units recognized at each site (six at VL-1 and four at VL-2), are identified on the basis of color, texture, morphology, and contact relations. The soil units at the Viking 2 site form a well-defined stratigraphic sequence, whereas the sequence at the Viking 1 site is only partially defined. The same relative soil colors occur at the two sites, suggesting that similar soil units are widespread on Mars. Several types of rock surface materials can be recognized at the two sites; dark, relatively 'blue' rock surfaces are probably minimally weathered igneous rock, whereas bright rock surfaces, with a green/(blue + red) ratio higher than that of any other surface material, are interpreted as a weathering product formed in situ on the rock. These rock surface types are common at both sites. Soil adhering to rocks is common at VL-2, but rare at VL-1. The mechanism that produces the weathering coating on rocks probably operates planet-wide.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 38
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    Eolian streaks in southwestern Egypt and similar features in the Cerberus region of Mars (1979)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Charting the southern seas - The evolution of the lunar Mare Australe (1979)
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    Publication Date: 2019-07-13
    Description: Mare Australe has been subjected to at least four major episodes of basalt eruption ranging in age from early Imbrian to Eratosthenian. The basalts were emplaced largely in flood eruptions from at least 197 vents located on post-basin impact crater floors. The youngest basalts occur in an annulus near the outer edge of the basin. The fill thickness apparently reflects a multiring structure for the post-impact morphology of the Australe basin; the thin basaltic fill was not sufficient a load to produce tectonic rilles, but mare ridges are present and exhibit a prominent north-south alignment.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 40
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    Multispectral mapping of the Apollo 15-Apennine region - The identification and distribution of regional pyroclastic deposits (1979)
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    Publication Date: 2019-07-13
    Description: Multispectral mapping of the Apollo 15-Apennine region has allowed the identification of numerous dark mantle deposits of probable pyroclastic origin. The deposits display a low albedo, appear to mantle and slightly subdue subjacent terrain, are spectrally distinct on the multispectral maps (high in the infrared but low in the ultraviolet) and generally exhibit a weak depolarized 3.8 cm radar echo. These characteristics are consistent with an origin by pyroclastic eruption. The regional dark mantle deposits are commonly associated with vents along marginal fractures and faults near the base of the Apennines, thereby emphasizing the role of basin-controlled weaknesses in providing channels for the upward migration of magma generated at depth. The spectral properties of the pyroclastic deposits are incompatible with those of Apollo 15 green glass but the deposits may be composed of material similar to the Apollo 15 brown or yellow glass. If so, the widespread distribution of the deposits suggest that mare basalts genetically related to the brown or yellow glass may occur in the Apollo 15 region. Moreover, pyroclastic volcanic activity has apparently been a more important and widespread process in the Apollo 15-Apennine region than has previously been thought.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 41
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    Mare Crisium geologic units - Implications of additional remote sensing data (1979)
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    Publication Date: 2019-07-13
    Description: Additional spectral reflectance data are presented for the Mare Crisium region. This new remote sensing information supports and supplements the subdivision of Mare Crisium into three major basalt units and shows further that: (1) the Luna 24 landing site is on a small region apparently surrounded by distinctly different units, but is clearly correlated with basalt Group IIA of Head et al. (1978); (2) exposures of Group IIB basalt in the northern and southern parts of the basin are spectrally similar; and (3) Group I basalts along the eastern part of the basin, which have been proposed to be relatively young (Boyce and Johnson, 1977), are spectrally similar to older Group I basalts.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 42
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    Thickness of the western mare basalts (1979)
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    Publication Date: 2019-07-13
    Description: The basalts of the western maria occupy large circular basins and surrounding lowlands associated with the basins. Mare Imbrium and Mare Humorum are the only well-preserved circular basins. Isopach mapping suggests that the vast expanse of basalt plains of Oceanus Procellarum mantles a composite structure of several coalescing basins. The thickest basalts are found in Mare Imbrium, Mare Humorum, and in the western part of the Oceanus Procellarum. Relatively thin basalts are found south and southwest of Mare Imbrium, in the Central Lowland region, and in northern Procellarium. For the most part, the general conclusions of earilier studies of the eastern maria are confirmed in the western maria.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Endogenic craters on basaltic lava flows - Size frequency distributions (1979)
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    Publication Date: 2019-07-13
    Description: Circular crater forms, termed collapse depressions, which occur on many basalt flows on the earth have also been detected on the moon and Mars and possibly on Mercury and Io. The admixture of collapse craters with impact craters would affect age determinations of planetary surface units based on impact crater statistics by making them appear anomalously old. In the work described in the present paper, the techniques conventionally used in planetary crater counting were applied to the determination of the size range and size frequency distribution of collapse craters on lava flows in Idaho, California, and New Mexico. Collapse depressions range in size from 3 to 80 m in diameter; their cumulative size distributions are similar to those of small impact craters on the moon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 44
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    Evidence for ancient mare volcanism (1979)
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    Description: The results of the present study suggest that dark-haloed impact craters are indicative of excavated mafic materials, originally emplaced as volcanic units, but subsequently buried by impact ejecta deposits from large craters and basins. Consequently, mapped light plains units should be viewed as soil units that may not reflect the origin of the underlying rock. Some observations which support these conclusions are examined.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 45
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    Alphonsus-type dark-halo craters - Morphology, morphometry and eruption conditions (1979)
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    Publication Date: 2019-07-13
    Description: The Alphonsus dark-halo craters are sites of volcanic eruptions with a characteristic crater radius of approximately 1 km. They are characterized by dark haloes ranging from 3 to 4 km, by substantial amounts of nonjuvenile material within the deposits, and by a lack of any associated lava flows or prominent constructional features, such as cones or domes. In the present paper, possible eruption styles are analyzed, using these observational constraints. It is concluded that an eruption process analogous to terrestrial volcanian explosive activity provides the most reasonable explanation for the characteristics of the deposits. The dark-halo craters appear to have formed contemporaneously with the emplacement of lavas in the adjacent Mare Nubium.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 46
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    Monogenetic volcanoes of the terrestrial planets (1979)
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    Description: Monogenetic volcanic activity has produced cinder cones and small shield volcanoes on the earth, moon, and Mars. Extraterrestrial cinder cones have median volumes only 25% as large as average terrestrial cinder cones, implying that their magma chambers are smaller and shallower (1 km depth vs 3 km). Ejection velocities for lunar and Martian cinder cones range from 20 to 70 m/sec, only 1/3 to 1/10 as high as for equal volume terrestrial eruptions. These low velocities imply low volatile contents for both Martian and lunar magmas.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 47
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    The chronology of the martian volcanoes (1979)
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    Publication Date: 2019-07-13
    Description: The volcanoes of Mars have been divided into three groups based on morphology: basaltic shields, domes and composite cones, and highland patera. A fourth group can be added to include the volcano-tectonic depressions. Using crater counts and the absolute chronology of Soderblom, an attempt is made to estimate the history of the volcanoes. Early in the martian history, about 2.5 b.y. ago, all three styles of volcanoes were active at various locations on the surface. At approximately 1.7-1.8 b.y. ago a transition occurred in the style and loci of volcanic construction. Volcanoes of younger age appear to be only of the basaltic shield group and are restricted to the Tharsis region. This same transition was noted by a change in the style of the basaltic shield group. Older shields were small low features, while the younger shields are significantly broader and taller.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 48
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    Meteorite impact in the ocean (1979)
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    Description: In the present study, the dynamic of hypervelocity impacts and crater formation in water are examined with allowance for the unique properties of water. More precisely, the transient crater calculated is permitted to relax and act as a source of oceanic surface waves.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 49
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    Effects of lift force on ejecta transport (1979)
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    Description: The possible effects of lift on individual ejecta trajectories after an impact event are examined, considering a dimensionless transport parameter (K), the initial velocity vector of the particles, and the ratio of the lift to drag coefficients. If this ratio is not equal to zero, the trajectory is greatly influenced by the lift coefficient, particularly for large values of K and high launch angles. It is suggested that lift potentially can affect small ejecta in the size range also affected by aerodynamic drag, thereby adding complexity to atmospheric effects discussed by Schultz and Gault (1978).
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    The history of an atmosphere of impact origin (1979)
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    Description: Most of the masses accreting onto the earth and terrestrial planets impacted at sufficiently high velocities to release their volatiles into the atmosphere by impact-heating. However, based on models of planetary growth by accumulation from solid bodies, the time-scale for accretion was sufficiently long that the average surface temperatures could not have risen above 320 K. Using measured reaction rates, the released volatiles should have been re-incorporated into the planet by hydrating the surface minerals and were subsequently buried during accretion. Rapid hydration of impact products precludes the formation of a thick atmosphere as the planet accreted. Thus, only the subsequent differentiation and evolution of the terrestrial planets determined the size and composition of each planet's atmosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Calculational investigation of impact cratering dynamics - Early time material motions (1979)
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    Description: Early time two-dimensional finite difference calculations of laboratory-scale hypervelocity (6 km/sec) impact of 0.3 g spherical 2024 aluminum projectiles into homogeneous plasticene clay targets were performed and the resulting material motions analyzed. Results show that the initial jetting of vaporized target material is qualitatively similar to experimental observation. The velocity flow field developed within the target is shown to have features quite similar to those found in calculations of near-surface explosion cratering. Specific application of Maxwell's analytic Z-Model (developed to interpret the flow fields of near-surface explosion cratering calculations), shows that this model can be used to describe the flow fields resulting from the impact cratering calculations, provided that the flow field center is located beneath the target surface, and that application of the model is made late enough in time that most of the projectile momentum has been dissipated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 52
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    Impact melting early in lunar history (1979)
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    Description: The total amount of impact melt produced during early lunar history is examined in light of theoretically and experimentally determined relations between crater diameter (D) and impact melt volume. The time dependence of the melt production is given by the time dependent impact rate as derived from cratering statistics for two different crater-size classes. Results show that small scale cratering (D less than or equal to 30 km) leads to melt volumes which fit selected observations specifying the amount of impact melt contained in the lunar regolith and in craters with diameters less than 10 km. Larger craters (D greater than 30 km) are capable of forming the abundant impact melt breccias found on the lunar surface. The group of large craters (D greater than 30 km) produces nearly 10 times as much impact melt as all the smaller craters, and thus, the large impacts dominate the modification of the lunar surface. A contradiction between the distribution of radiometric rock ages and a model of exponentially decreasing cratering rate going back to 4.5 b.y. is reflected in uncertainty in the distribution of impact melt as a function of time on the moon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Monte Carlo simulation of lunar megaregolith and implications (1979)
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    Publication Date: 2019-07-13
    Description: A realistic Monte Carlo model closely simulating the evolution of the lunar megaregolith over a large area of 67 million sq. km of the front surface of the moon is presented. Craters larger than 100 km in diameter observed over the entire surface of the moon and those less than 100 km lying in the referenced area are included in the simulation. A total of 21,664 craters are processed. The model predicts the average thickness of the megaregolith to be about 1.9-2.0 km. Curves for the variation of the regolith thickness across the simulated area are given and show that about 50% of the area is covered with regolith less than 1 km thick. The model produces crater structures similar to the ones observed in the lunar highlands, it partially supports the layering theory for crater structures that the variations in strength and density of target materials may be responsible for the observed differences in the morphologies of lunar craters, and rules out the possibility that all craters when formed are bowl-shaped with a fixed depth/diameter ratio characteristic of small craters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Ejecta emplacement of the Martian impact crater Bamburg (1979)
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    Description: The paper examines the ejecta emplacement of the Martian impact crater Bamburg. During ejecta emplacement, secondary crater formation preceeded the deposition of mobile surface flows, which are overrun by more viscous flows characterized by longitudinal grooves and transverse ridges. Many areas of flat terrain on the ejecta deposits may indicate that the sediment-laden melt water percolated out of the volatile-rich ejecta and the crater rim. The number of secondary craters associated with Bamburg is less than one third the value for lunar and Mercurian craters of equivalent size; this is attributed to preferential destruction of ejecta blocks sufficiently large to form secondary craters or to the subsequent burial of such craters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 55
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    Large impact basins on Mercury and relative crater production rates (1979)
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    Description: A search for impact basins on Mercury having diameters greater than 200 km revealed evidence for 40 such structures on the 47% of Mercury mapped at sufficient resolution by Mariner 10. This is similar to the number (35) found by Schaber et al. (1977), although there is disagreement in the details of both diameters (for basins observed by them and by the authors) and in the existence of individual basins. The differences are described in detail. A log (cumulative number/unit area)-log (diameter) plot for mercurian basins has a least squares slope of -2; basins show somewhat less scatter about this line than do the Schaber et al. basins. Mercury has (in cumulative number/unit area) only 37% as many basins as does the moon over the entire range of diameters greater than 300 km. If both the moon and Mercury have had similar preservation times for craters and if common populations of impactors are involved, then Mars-crossers may have been a dominant contribution to the basin-forming objects.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Mercurian crater rim heights and some interplanetary comparisons (1979)
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    Description: Rim height (Re) data have been gathered through shadow measurements for 30 fresh mercurian craters with diameters (D) between 2.6 and 39 km. Small mercurian craters (i.e., those less than about 16 km in diameter) have higher rims than do lunar craters of the same diameter; on the basis of Re/D measurements alone, however, mercurian craters larger than about 16 km appear to be indistinguishable from their lunar counterparts (those greater than about 21 km in diameter). Apparent crater depths (Ra, the crater depth measured from the initial target surface) derived from empirical data allude to a decrease in Ra/D with calculated modal impact velocity. This is consistent with the hypothesis that higher impact velocities place the effective depth of burst of the event closer to the surface, thus causing a shallower crater.
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    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 57
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    Asymmetric terracing of lunar highland craters - Influence of pre-impact topography and structure (1979)
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    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 58
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    Smythii basin topography and comparisons with Orientale (1979)
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    Description: The Smythii basin has the most extensive topographic coverage of any lunar multi-ringed basin. Topographic data are used to study the morphology and morphometry of Smythii and to make comparisons with similar basins. The depth of the basin is shown to be over 8 km, which is comparable to that of Orientale. The inner ring reaches heights of 3.4 km, while the intermediate ring exhibits little relief. Lowest points in the basin are related to mare ridges. Basin volume is estimated to be 21 million cubic kilometers. Evidence suggests that significant differences in substrate characteristics may have existed for the Smythii and Orientale impacts.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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    Central peaks in lunar craters - Morphology and morphometry (1979)
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    Description: Fresh lunar craters with diameters from 17 to 175 km are found to display a linear relationship between the central peak morphology and morphometry and such critical crater parameters as rim crest diameter, floor diameter, and substrate. Some other previously established linear relationships have been cited as evidence that floor diameter, peak height, and peak ring diameter are related to the kinetic energy of impact. The two new relations derived in the present work would therefore indicate that the central peaks, too, are related to the kinetic energy of impact, and probably begin to form early in the cratering event as suggested by Milton and Roddy (1972) and Head (1978). There seems to be no obvious reason to expect such linear relationships between central peak diameter and rim crest and floor diameter if the peaks are formed by gravity induced failure of the transient cavity, as suggested by Dence et al. (1968).
    Keywords: LUNAR AND PLANETARY EXPLORATION
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    Experimental shock metamorphism of mono- and polycrystalline olivine - A comparative study (1979)
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    Description: The paper reports on a series of controlled shock recovery experiments which have been performed on over 40 samples including monocrystalline, polycrystalline, dunite, and porous particulate olivine-bearing targets. Results of the mineralogical and petrological analyses of these samples are used to establish a general and comparative diagnosis of shock effects generated in various olivine-bearing materials. Finally, some experiments are conducted under different ambient pO2 conditions so that information on the distribution of observed impact features is derived as a function not only of peak pressure and texture of the target sample, but also of specific environmental conditions.
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    Structural deformation at the Flynn Creek impact crater, Tennessee - A preliminary report on deep drilling (1979)
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    Publication Date: 2019-07-13
    Description: The geologic and core drilling studies described in the present paper show that the Flynn Creek crater has such distinctive morphological features as a broad flat hummocky floor; large central peak; locally terraced crater walls; uplifted, as well as flat-lying rim segments; and a surrounding ejecta blanket. The major structural features include a shallow depth of total brecciation and excavation as compared with apparent crater diameter; a thin breccia lens underlain by a thin zone of disrupted strata; concentric ring fault zones in inner rim, beneath crater wall, and outer crater floor regions; a large central uplift underlain by a narrow dipping zone of deeply disrupted strata; faulted, folded, brecciated, and fractured rim strata; and uplifted rim strata, which dip away from the crater, and flat-lying rim strata, which terminate as inward dipping rocks.
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    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Petrology of impactites from Lake St. Martin structure, Manitoba (1979)
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    Publication Date: 2019-07-13
    Description: The 23-km Lake St. Martin crater was produced 200 to 250 million years ago in Archean granitic to amphibolic gneiss, overlain by 400 to 500 m of Ordovician to Devonian limestone and dolomite. In the present paper, a schematic model of the field geology, petrology, and geochemistry is presented. The scenario is built in part on the calculations of Kieffer and Simonds and observations made on the Lake St. Martin structure.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Shock metamorphism of granulated lunar basalt (1979)
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    Publication Date: 2019-07-13
    Description: The paper deals with an extensive series of shock-recovery experiments performed on both nonporous crystalline basalt and its granulated and sieved counterpart to study the role of porosity and grain size in shock motomorphic effects under otherwise identical conditions. Shocked samples are compared with unshocked starting material in terms of textural and mineralogical modifications attributable to shock. A comparative petrographic and chemical characterization is presented of pulverized and sieved lunar basalt 75035 shocked between 6 and 75 GPa in comparison with holocrystalline disks of the same basalts shocked in 10 earlier experiments. Specifically, a petrographic classification of shock features is given, along with an estimation of relative amounts of shock glasses and a chemical characterization of shock glasses in each shocked granular basalt.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 64
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    Elastic lithosphere thickness on the moon from mare tectonic features - A formal inversion (1979)
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    Publication Date: 2019-07-13
    Description: The thickness (T) of the lunar elastic lithosphere at the time (3.6 to 3.8 billion years ago) of the earliest preserved basalt flows in circular mare basins can be estimated by inverting the observed locations of extensional tectonic features in and surrounding the maria. In performing the inversion, the lithosphere is modeled as an elastic shell with a liquid interior, and the basalt load for each mare is approximated by a set of concentric cylinders. To permit solving the forward problem of placing radial limits on the positions of the rilles around a given mare, an additional parameter F, the ratio of the radial stress at the radial limits to the maximum radial stress, is introduced. T and F are chosen to give the best weighted-squares fit of the radial limits to the observations, and are used as the initial values in a linearized matrix inversion to check the resolution and estimate errors. The application of the procedure to three maria with prominent extensional features, Humorum, Orientale, and Serenitatis, gives values of T from about 40 + or - 10 to 50 + or - 10 km, and in each case the linearized matrix equation has an exact inverse.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 65
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    Some possible effects of solid-state deformation on the thermal evolution of ice-silicate planetary bodies (1979)
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    Publication Date: 2019-07-13
    Description: Several ways in which solid-state deformation could be important in the evolution of an ice-silicate body are considered. The considerations suggest several scenarios for the evolution of Ganymede and Callisto which might be tested on the basis of Voyager and Galileo results. Several potential sources of heat may have caused extensive melting early in the history of these bodies, including a high initial luminosity of Jupiter, accretional heating, gravitational segregation of ice and silicates in a homogeneously accreted body, and deformation by synchronous rotation. The analysis leads to the conclusion that two mechanisms - diapirism and solid-state convection - could be sufficient to inhibit the development of an excessive liquid water mantle, or to cause refreezing of such a mantle formed prior to steady-state conditions or from other heat sources.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 66
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    The lunar interior - A summary report (1979)
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    Publication Date: 2019-07-13
    Description: The complete seismic data set collected by the Apollo network contains about 40 events which provide significant structural information on the lunar interior. The seismograms from these events yield a set of direct wave arrival times that constitutes the most reliable information on the seismic structure of the moon. Secondary data include possible reflected arrivals from crustal and mantle interfaces, an apparent shear wave shadow zone for surface events beginning at about 90 deg distance, and the shear wave amplitude decay with distance. Analysis of these data give well-constrained and stable average velocity values for the upper and lower mantle regions independent of most assumptions. The upper-lower mantle transition can begin no shallower than 400 km depth and may represent a compositional change although the effects of increased temperature cannot be ruled out.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 67
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    The bounds of the heat production rate within the moon (1979)
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    Publication Date: 2019-07-13
    Description: A new approach is proposed to the evaluation of the lower and upper bounds of the global heat production rate within planetary interiors. The approach is based on the relationship between the internal energy change and the volume change of a planetary object. For illustration, the approach is applied to the moon. Using an average global surface heat flux of 18 erg/sq cm-sec, and assuming constancy of the lunar radius during the past 3.2 billion years. the lunar heat release within the past 3.2 billion years is estimated at (30 to 40) x 10 to the tenth erg/cu cm. This is equivalent to the present day uranium concentration of 35 to 50 ppb provided the radiogenic isotopes are of the same proportion as that given by Toksoz et al. (1978).
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 68
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    Parameterized convection within the moon and the terrestrial planets (1979)
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    Publication Date: 2019-07-13
    Description: For a fluid layer or a self-gravitating fluid sphere uniformly heated from within, the internal temperature can be parameterized in terms of the appropriate Rayleigh number. The heat generation term includes both radioactive heat release and transient heating or cooling. This parameterization has been verified by comparisons with laboratory experiments. Thermal history calculations have been carried out for the earth, Venus, Mars, Mercury, and the moon. The results for the earth and Venus indicate that two scales of convection are occurring, one including the surface plates and the second occurring beneath the surface plates. In all cases the present heat flows are between seven and twelve per cent greater than the values obtained assuming a steady state balance between heat flow and internal heat generation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 69
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    Electrical conductivity of the lunar interior - Theory, error sources, and estimates (1979)
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    Publication Date: 2019-07-13
    Description: Estimates of the electrical conductivity of the lunar interior were previously obtained by comparison of magnetometer data at the lunar surface and in near lunar space. In studies based on solar wind observations, IR was assumed that fields induced in the lunar interior by time-varying external fields are confined by the solar wind within the lunar interior on the dayside and within a cylindrical plasma cavity on the nightside. In the present paper, the induced fields are calculated for a more realistic conical plasma cavity geometry.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 70
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    Comparison of theoretical and observed 3.55 cm wavelength brightness temperature maps of the full moon (1979)
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    Publication Date: 2019-07-13
    Description: In the present paper, a map of the moon's 3.33-cm thermal emission, constructed from observation data, is compared with a map calculated from a detailed model for regolith properties. In an 'observed minus predicted' difference map, two distinct anomalies, each approximately 2 K warmer than their surroundings, are detected. The anomalies are smaller in areal extent than the maria in which they are located (Tranquillitatis and Imbrium). A preliminary analysis, based on calculations of the effects of model parameters on observed brightness temperature, indicates that the two 'hotspots' can be explained by postulating that they are regions possessing a 30 to 40 percent higher than moon-average opacity and that their profile of physical temperature with depth is not necessarily anomalous. On a global scale, a pattern of 'maria warmer than highlands' is presented which exhibits a brightness temperature contrast of approximately 5 K.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 71
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    Models of an early lunar dynamo (1979)
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    Publication Date: 2019-07-13
    Description: The hypothesis that a dynamo once existed in the moon, and hence was the source of lunar paleomagnetism, is tested using a model for the global thermoremanent magnetization of spherical lithospheres. Various models of an ancient lunar dipole field are used which incorporate intensity variations and reversals, and which are consistent with lunar sample paleointensities. It is found that non-reversing lunar dynamos which have simple exponential decay histories beginning at 4.6 b.y. ago are inconsistent with this limit, unless the moon has been thoroughly demagnetized to a depth of tens of kilometers by impacts or other processes. An early lunar dynamo cannot be excluded by global scalar measurements unless the permanent lunar dipole moment is shown to be significantly less than 10 to the 13th power G/cu cm by future spacecraft measurements, which may be technologically impossible; vector measurements of lunar magnetic anomalies over the whole moon offer a possibility of determining the source of the field which magnetized the lunar crust.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 72
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    Shallow moonquakes - Depth, distribution and implications as to the present state of the lunar interior (1979)
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    Publication Date: 2019-07-13
    Description: The observed seismic amplitudes of HFT (high-frequency teleseismic) events do not vary with distance as expected for surface sources, but are consistent with sources in the upper mantle of the moon. Thus, the upper mantle of the moon is the only zone where tectonic stresses deriving from differential thermal contraction and expansion of the lunar interior are presently high enough to cause moonquakes. The distribution of shallow moonquake epicenters suggests a possible correlation with impact basins, implying a lasting tectonic influence of impact basins long after their formation. The finite depths now assigned to these shallow moonquakes necessitate further revision to the seismic structural model of the lunar interior.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 73
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    Electrical conductivity anomalies associated with circular lunar maria (1979)
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    Publication Date: 2019-07-13
    Description: A strong anisotropy is observed in magnetic field fluctuations measured by the Lunokhod 2 magnetometer located on the eastern edge of Mare Serenitatis. This anisotropy can be explained by a regional anomaly in the subsurface electrical conductivity distribution associated with the mare similar to the proposed conductivity anomaly associated with Mare Imbrium. The Serenitatis magnetic field anisotropy is compared to the field fluctuation measured by the Apollo 16 magnetometer 1100 km to the south, and this comparison indicates that the subsurface conductivity distribution can be modeled by a nonconducting layer in the lunar lithosphere which is 150 km thick beneath the highlands and 300 km thick beneath Serenitatis. The decrease in electrical conductivity of the upper mantle beneath the mare may result from lower temperatures due to transport of thermal energy and radioactive heat sources to the surface during mare flooding. This proposed anomaly, along with that proposed for Mare Imbrium, strengthens the possibility of regional anomalies in electrical conductivity associated with all circular lunar maria.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 74
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    Initial Pioneer Venus magnetometer observations (1979)
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    Description: Initial Pioneer Venus magnetometer observations reveal a highly dynamic interaction between the solar wind and the ionosphere and a very weak and possibly absent intrinsic magnetic field. The bow shock position and the altitude of the ionopause vary markedly from day to day. The magnetic pressure in the magnetosheath just outside the ionopause is in near balance with the thermal ionospheric pressure inside. Although the ionospheric magnetic field strength is generally low, occasional enhancements are observed with field strengths exceeding that in the magnetosheath. These bundles of magnetic flux, or flux ropes, may be convected to the night side ionosphere in which large field strengths (compared to the dayside) are common. The magnetic field magnitude and direction in this region are quite variable, suggesting that the field is not due to an intrinsic planetary source, but rather due to induced ionospheric currents. The magnetic moment is probably much less than 10 to the 22nd Gauss-cu cm.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 75
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    High spatial resolution measurements of surface magnetic fields of the lunar frontside (1979)
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    Publication Date: 2019-07-13
    Description: Using 0.5 keV electron reflection measurements from real time tracking of the Apollo 15 and 16 Subsatellites the surface fields were mapped on the lunar frontside. Although the surface coverage is poor except near the Apollo 16 Subsatellite track, over 100 distinct regions of greater than 0.2 square degrees area with maximum surface field strength equal to or greater than 12 nT were identified. Preliminary contour maps of two of the largest regions and the Reiner Gamma region observed by the orbiting magnetometer are presented.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Gravity anomaly and structure associated with the Lamont region of the moon (1979)
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    Publication Date: 2019-07-13
    Description: Lamont is a unique lunar feature in southwestern Mare Tranquillitatis associated with radial and concentric ridge patterns and a positive free-air gravity anomaly. Best fitting models to high and low altitude gravity data place nearly all of the anomalous mass in the subsurface, consistent with the hypothesis that Lamont is a mascon. Lamont is positioned on the axis of a 1500 m deep north-south topographic trough occupying western Mare Tranquillitatis. It is proposed that this trough is a synclinal fold in the lunar crust and the tectonic fabric of western Tranquillitatis is consistent with the superposition of the stress fields due to synclinal folding and the loading of the lithosphere by the Lamont mascon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 77
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    Lunar nearside magnetic anomalies (1979)
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    Publication Date: 2019-07-13
    Description: Contour maps of the vector components of the lunar crustal magnetic field measured with the Apollo 16 subsatellite magnetometer at low altitudes across the central near side are presented. A solution was obtained for a minimum mean magnetization level of about 700 times the stable magnetization component of the most magnetic returned lunar crustal samples. Attention is given to the Reiner Gamma anomaly that is found to represent macroscopic evidence for a surficial darkening process that is dominantly solar wind-dependent.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 78
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    On the natural remanent magnetism of certain mare basalts (1979)
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    Publication Date: 2019-07-13
    Description: The natural remanent magnetization (NRM) and magnetic properties of five fine-grain mare basalts were investigated. The NRM of two vitrophyres has a large soft component, and the directional stability during AF demagnetization is poor. The remaining samples have NRM which is too soft to be of thermal origin and yet too hard to be simply isothermal contamination. It is suggested that the NRM of the samples could be shock remanent magnetization.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 79
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    Paleointensity determinations at elevated temperatures - Sample preparation technique (1979)
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    Description: A technique has been developed for the encapsulation of rock samples in order to prevent the chemical alterations which commonly accompany paleointensity measurements at elevated temperatures. The technique involves vacuum pumping at about 100 C of the sample as placed in a silica tube. The tube containing the sample and a Ti 'getter' are sealed under vacuum. Measurements can be made at 200 and 300 C. Immediately after this, the sample is sealed-off from the getter. The sample is now ready for measurements at higher temperatures.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 80
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    Microwave dielectric measurements of lunar soil with a coaxial line resonator method (1979)
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    Description: A method is given for sensitive dielectric measurements at a series of microwave frequencies using a section of coaxial line. The line is used as a 1-port cavity resonator; it resonates when the electrical length of the center conductor equals 1, 2 . . . , N half-wave lengths. The dielectric properties of an Apollo 17 dried soil sample were measured in vacuum over a temperature range of 173 to 373 K. The relative permittivity and the loss tangent were determined and the frequency dependence was very small. The derivative with respect to temperature, per degree, was 0.00045 for the permittivity and 0.00002 for the loss tangent.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: PB80-178858 , Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Comparison of single crack propagation in lunar analogue glass and the failure strength of rocks (1979)
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    Publication Date: 2019-07-13
    Description: New data of crack propagation in lunar analogue glass provides important input for the construction of deformation maps (maps which delineate the rates and principal means of material deformation under various environmental conditions) applicable to the lunar crust. Comparison of single crack propagation data obtained on flat plates of glass and failure strength data obtained on fine grained rock samples show that single crack propagation velocities are directly related to the failure strength of rocks. The chemical reaction between water and silicon-oxygen bonds at the crack tip seems to be of first order. This greatly simplifies extrapolation to low partial pressures of H2O
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 82
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    Time dependent deformation of a basalt at low differential stress (1979)
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    Description: A detailed study of linear elastic deformation in Ralston basalt during triaxial loading has been made as a function of strain rate (8 x 10 to the -8th per sec to 5 x 10 to the -5th per sec) and moisture content under constant confining pressure (500 bars) and temperature (20 C). Young's modulus was found to be constant and independent of moisture content and strain rate; however, Poisson's ratio decreased 5.7 plus or minus 1.6% and 6.7 plus or minus 1.6% per order of magnitude increase in strain rate for two suites of dry samples and 1.4 plus or minus 1.2% per equivalent change in strain rate for one suite of wet rocks. Lateral expansion in dry rocks is therefore a more sensitive function of strain rate than it is in wet rocks. It is suggested that this strain-rate dependence is related to microcracking.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Compressional velocity measurements for a highly fractured lunar anorthosite (1979)
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    Description: The compressional wave (V sub p) velocities in three mutually perpendicular directions have been measured in lunar sample 60025,174, lunar anorthosite. V sub p measurements were made at ambient temperature and pressure and a new technique was developed to measure the velocities because of the tremendous acoustic wave attenuation of the lunar sample. The measured velocities were all less than 1 km/sec and displayed up to a 21% departure from the mean value of the three directions. The velocities agree with seismic wave velocities determined for the lunar surface at the collection site.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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    Lunar and Planetary Science Conference, 10th, Houston, Tex., March 19-23, 1979, Proceedings. Volume 3 - Planetary interiors and surfaces (1979)
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    Description: The areas covered on the present symposium include geophysical investigations based on laboratory and planetary measurements; impact and volcanic processes; and planetary surface features and processes. The topics discussed include models of an early lunar dynamo, parameterized convection within the moon and the terrestrial planets, the bounds of the heat production rate with the moon, the shock metamorphism of granulated lunar basalt, asymmetric terracing of lunar highland craters, large impact basins on Mercury, impact melting in early lunar history, and evidence for ancient mare volcanism.
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    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 85
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    Complex igneous processes and the formation of the primitive lunar crustal rocks (1979)
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    Description: Crystallization of a magma ocean with initial chondritic Ca/Al and REE ratios such as proposed by Taylor and Bence (TB, 1975), is capable of producing the suite of primitive crustal rocks if the magma ocean underwent locally extensive assimilation and mixing in its upper layers as preliminary steps in formation of an anorthositic crust. Lunar anorthosites were the earliest permanent crustal rocks to form the result of multiple cycles of suspension and assimilation of plagioclase in liquids fractionating olivine and pyroxene. There may be two series of Mg-rich cumulate rocks: one which developed as a result of the equilibration of anorthositic crust with the magma ocean; the other which formed in the later stages of the magma ocean during an epoch of magma mixing and ilmenite crystallization. This second series may be related to KREEP genesis. It is noted that crystallization of the magma ocean had two components: a low pressure component which produced a highly fractionated and heterogeneous crust growing downward and a high pressure component which filled in the ocean from the bottom up, mostly with olivine and low-Ca pyroxene.
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    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 86
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    Effects of pressure on the crystallization of a 'chondritic' magma ocean and implications for the bulk composition of the moon (1979)
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 87
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    Lunar basalts and pristine highland rocks - Comparison of siderophile and volatile elements (1979)
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    Description: The objective of the present paper is to compare pristine highland rocks and low-Ti mare basalts on the basis of all 53 Chicago analyses of these to types of rock. Apart from being of interest in its own right, such a comparison provides a test of Delano and Ringwood's (1979) contention that 'abundances of Ge, Au, and other siderophile elements in pristine highland rocks are not consistent with magmatic differentiation'. The other topics reexamined in this paper are the correlation of siderophiles and volatiles in pristine rocks with Rb and Cs (likewise questioned by Delano and Ringwood), the relationship of 'non-mare' basalts (14053, 60639) to their mare counterparts, and the abundance of some incompatible elements in the lunar bulk.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 88
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    Seismic Q and velocity at depth (1979)
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    Description: Measurements of the p-wave and s-wave internal friction quality factors (Q) and velocities of samples of a moderately outgassed terrestrial analog of lunar basalt exposed simultaneously to temperatures and hydrostatic confining pressures in accordance with the best available estimates of the lunar selenotherm are presented. Q values and velocities are found to increase with simulated depth, and an extrapolation of the Q value to a thoroughly outgassed states provides a Q value in reasonable agreement with those derived from lunar seismic data, suggesting a very dry lunar crust. Results also imply that similar seismic determinations for Mars would be able to distinguish between a dry crust and a crust containing water trapped beneath a layer of ice. Results of thermal cracking tests which demonstrate that high degrees of cracking associated with thermal cycling, as during the lunar day, are not inconsistent with high Q in a dry environment are presented, and it is shown that volatiles with diple moments comparable to H2O can greatly affect Q. Possible attenuation mechanisms are then considered, and velocity measurements on a synthetic anorthosite are presented.
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    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 89
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    Basaltic volcanism - The importance of planet size (1979)
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    Publication Date: 2019-07-13
    Description: The volumetrically abundant basalts on the earth, its moon, and the eucrite parent planet all have chemical compositions that are controlled to a large extent by dry, low-pressure, crystal-liquid equilibria. Since this generalization is valid for these three planetary bodies, we infer that it may also apply to the other unsampled terrestrial planets. Other characteristics of basaltic volcanism show variations which appear to be related to planet size: the eruption temperatures, degrees of fractionation, and chemical variety of basalts and the endurance of basaltic volcanism all increase with planet size. Although the processes responsible for chemical differences between basalt suites are known, no simple systematization of the chemical differences between basalts from planet to planet has emerged.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 90
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    The nature of asteroidal differentiation processes - Implications for primordial heat sources (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: A review of the geochemical data on basaltic achondrite group meteorites, here defined as diogenites, eucrites, howardites, mesosiderites, main-group pallasites and IIIAB irons, suggests that the following processes and properties were important in determining the compositions of igneous materials on asteroidal sized bodies: (1) inhomogeneities in source rock compositions, (2) variable degrees of partial melting from 5-100%, (3) multiple melt genesis from a single source region, (4) fractional crystallization, and (5) remelting of earlier formed igneous rocks. All of this activity started during or shortly after the major asteroidal accretion phase as suggested by the numerous 4.6 Gyr ages for eucrites and may have lasted for at least 200 m.y. The above properties imply an early, intense heat source that was both spatially and temporally variable. A review of asteroid thermal modeling for various heat sources shows that heating by short-lived Al-26 alone appears to be incapable of supplying the observed geochemical variations.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 91
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    Noble gas trapping and fractionation during synthesis of carbonaceous matter (1979)
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    Publication Date: 2019-07-13
    Description: An investigation of noble gas entrapment during synthesis of carbonaceous, macromolecular, and kerogen-like substances is presented. High molecular weight organic matter synthesized in aqueous condensation reactions contained little gas, and the composition was consistent with fractionation due to noble gas solubility in water; however, propane soot produced during a modified Miller-Urey experiment in an aritificial gas mixture contained high concentrations of trapped noble gases that displayed strong elemental fractionation from their reservoirs. It is concluded that theses experiemnts show that processes exist for synthesis of carbonaceous carriers that result in high noble gas concentrations and strong elemental fractionation at temperatures well above those required by absorption to achieve similar effects.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 92
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    Xenon from intermediate zones of supernovae (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The paper examines the photodisintegration and neutron capture in massive stars which show that the bulk of the p-isotopes of Xe is formed during the gamma-process of Woosley and Howard (1978) by stripping of the Xe + Be seeds. The environments in which the chondrites can be formed were determined by the neutron-capture calculations; they show that the Xe-124-rich gas must be associated at the sources with anomalously large overabundances of Nd-142, Sm-144, and possibly Ba-130, and with anomalously small overabundances of the p-isotopes of Se, Kr, Sr, and Mo.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 93
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    Mars - Large scale mixing of bright and dark surface materials and implications for analysis of spectral reflectance (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 94
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    Lunar multispectral imaging at 2.26 microns - First results (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The first results of line-scan imaging of the moon at 2.26 microns and 0.56 micron are presented. Among the many features observed in the 2.26 micron/0.56 micron ratio image, fresh rock and immature soils stand out as dark (i.e., low ratio) due to their infrared absorption bands. Also notable in this image are several strikingly bright (high 2.26 micron/0.56 micron ratio) areas which are likely to contain pyroclastic, glass-related materials. Some of these bright areas correspond to dark mantling material. Others (e.g., Sulpicius Gallus, Aristarchus Plateau) are distinctly different in their overall spectral reflectance and it is suggested that these localities contain varieties of pyroclastic glass-related materials which were not sampled by Apollo 17 but which are relatively abundant elsewhere on the moon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 95
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    Vacuum ultraviolet reflectance spectra of group H chondrites (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The spectral reflectances of seventeen group H chondrites have been measured in the vacuum ultraviolet region, from 5 to 14 eV photon energy (250 to 90 nm, wavelength), as part of a survey of all meteorite types. Olivines, ortho-, and clino- pyroxenes are the three most important silicate minerals in these meteorites, and the spectrum of each mineral contains a distinct peak caused by a transition believed to be excitonic in nature and involving the valence-conduction bandgap. The energy at which this peak occurs varies as a function of mineral composition, and this variation has been determined from the spectra of a number of mineral standards. The observed positions of the olivine and pyroxene peaks in the meteorite spectra are compared to predicted positions based on the standard minerals.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 96
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    Spectra of Fe-Ti silicate glasses - Implications to remote-sensing of planetary surfaces (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Optical spectra of synthetic Fe-Ti silicate glasses and the temperature variations of the spectral features were investigated. The spectra are assigned to absorptions due to crystal field (CF) transitions in Ti(3+), Fe(2+) in octahedral coordination, and Fe(2+) in tetrahedral coordination, and to metal-metal and oxygen-metal charge transfer (CT) transitions which contribute to the near ultraviolet absorption edge. Temperature variations of the optical bands have been studied to explore implications for remote sensing. Caution is urged in the use of the absorption edge as a measure of TiO2 concentrations on planetary surfaces and in regolith samples.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 97
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    Regional chemical variations in lunar basaltic lavas (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The higher Al2O3 concentrations in mare soils at Apollo landing sites, relative to mare basalts, have generally been attributed to the presence of 20-30% of terra material in the mare surface regolith. This viewpoint is shown to be erroneous when entire maria are studied; the amount of terra material in typical mare surface regoliths is only about 5%, or less. The bulk of the mare soils are the comminuted remains of aluminous mare basalt flows. On a regional scale, the sample and orbital data for maria define prominent chemical variations that are well beyond those expected from simple igneous processes and therefore indicate that gradations in one or more of the major parameters of planetary differentiation caused these variations. The increasingly abundant evidence for regional variations in the chemical compositions of lunar basalts requires that regional petrogenetic provinces must be considered in models of lunar evolution.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 98
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    Are early magnesium-rich basalts widespread on the moon (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Orbital X-ray data indicate that high-magnesium material systematically occurs along mare/terra boundaries in all the lunar nearside basins for which there is orbital X-ray coverage. These peripheral units appear to represent the earliest stages of volcanism within each of the basins, although they were not necessarily emplaced at the same time in lunar history. High-magnesium subsurface layers excavated by post-mare impact craters in central Mare Crisium and Mare Fecunditatis suggest that the peripheral units are the only visible edges of a basin-wide basalt layer, largely buried by younger less-magnesian flows. This evidence suggests that early magnesium-rich mare basalts are widespread on the moon and that their volumes may be greatly underestimated. Abundant early mare deposits of this type would place severe constraints on models of mare basalt petrogenesis.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 99
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    Evidence for early volcanism in mare Smythii (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The major geologic units in and around the Smythii basin are reflected in the Al2O3 and MgO values obtained using improved orbital X-ray fluorescence data from Apollo 15. One of these units is a high albedo plains-forming unit that has Al2O3 and MgO concentrations different from those of similar plains-forming units located in the terra west of Smythii and south of Crisium and also different from those of adjacent terra and mare materials. The chemical composition of the plainsforming unit suggests a volcanic origin; the inferred Al2O3 and MgO-rich nature of this presumed early volcanic material is supported by the fact that even the later, low albedo, lightly cratered mare fill in Mare Smythii has a high MgO value, and its Al2O3 concentration is higher than that of similar basaltic material in other maria.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 100
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    A comparison of mare surface titanium concentrations obtained by spectral reflectance and gamma-ray spectroscopy - An early assessment (1979)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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