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  • LUNAR AND PLANETARY EXPLORATION  (151)
  • ASTROPHYSICS  (74)
  • 1975-1979  (224)
  • 1970-1974  (1)
  • 1978  (224)
  • 1972  (1)
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  • 1975-1979  (224)
  • 1970-1974  (1)
Year
  • 1
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    Martian atmosphere modeling between 0.4 and 3.5 microns - Comparison of theory and experiment (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: A model of the lower atmosphere of Mars has been constructed that combines aerosol absorption and scattering with a line-by-line analysis of CO2 and H2O in a multilayer radiative transfer program. Aerosol composition previously inferred from the NASA Lear Jet Observatory data was used to measure the optical complex indices of refraction of appropriate Martian analogs from 0.4 to 2.5 microns. The aerosol vertical particle density scale was deduced using the Viking camera observations of the soil and sky intensities between 0.4 and 1.0 microns in comparison with those modeled using a multilayer Mie scattering program. A comparison of observed Mars atmospheric absorptions was made with those obtained using Lorentz, Voigt, and Doppler line profiles in a multilayer model of the CO2 and H2O. The Voigt line profile of CO2 absorption at approximately 4976 kaysers was then combined in a multilayer aerosol model of the Martian atmosphere. An evaluation of the effect on the line shape was made using several aerosol loadings.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: In: Symposium on Planetary Atmospheres; Aug 16, 1977 - Aug 19, 1977; Ottawa; Canada
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    The radii of Uranian rings alpha, beta, gamma, delta, epsilon, eta, 4, 5, and 6 from their occultations of SAO 158687 (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: All available timing data for the occultations of SAO 158687 on March 10, 1977, by the cited rings of Uranus are analyzed. Least-squares fits to the data are performed using a model which postulates that rings alpha, beta, gamma, and delta are circular and coplanar. A solution obtained under the assumption that the ring plane coincides with the plane of the satellite orbits is adopted which yields radii of 44,844 km for ring alpha, 45,799 km for ring beta, 47,746 km for ring gamma, and 48,423 km for ring delta. The uncertainties in these values are discussed along with the apparent shapes and inclinations of these main rings. The mean radii estimated for the other rings are: 47,323 km for ring eta, 42,663 km for ring 4, 42,360 km for ring 5, and 41,980 km for ring 6.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Astronomical Journal; 83; Aug. 197
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    Conclusions derived from the evidence on accretion in meteorites (1978)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: A study of the evidence on accretion in meteorites shows that gross chemical features of chondritic meteorite type were established by accretion of materials with characteristic chemical and isotopic compositions. Some meteorites have been subjected to intensive mechanical and/or thermal processes. Mixing has occurred among meteorite types, presumably late in the accretion sequence. From the materials which appear to have escaped substantial modification it can be concluded that the relative velocities between accreting grains varied but in some cases were very low. Accretion took place after most, if not all, of the gaseous components had been separated from the condensed portion of solar matter.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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    NASA TECHNICAL REPORTS
  • 4
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    Crustal evolution inferred from Apollo magnetic measurements (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Magnetic field and solar wind plasma density measurements were analyzed to determine the scale size characteristics of remanent fields at the Apollo 12, 15, and 16 landing sites. Theoretical model calculations of the field-plasma interaction, involving diffusion of the remanent field into the solar plasma, were compared to the data. The information provided by all these experiments shows that remanent fields over most of the lunar surface are characterized by spatial variations as small as a few kilometers. Large regions (50 to 100 km) of the lunar crust were probably uniformly magnetized during early crustal evolution. Bombardment and subsequent gardening of the upper layers of these magnetized regions left randomly oriented, smaller scale (5 to 10 km) magnetic sources close to the surface. The larger scale size fields of magnitude approximately 0.1 gammas are measured by the orbiting subsatellite experiments and the small scale sized remanent fields of magnitude approximately 100 gammas are measured by the surface experiments.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-78524 , A-7608
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 5
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    Infrared observations of asteroids from earth and space (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Infrared reflectances at wavelength between 1 and 4 micrometers are used for determining asteroid surface mineralogy, surface composition, diameters, and albedos. Thermal models were developed for analyzing infrared observations at longer wavelengths. The discovery of a spectral feature due to water of hydration on Ceres seems to contradict the mineralogy inferred from spectrophotometry.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Asteroids; p 127-144
    Format: application/pdf
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  • 6
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    Interplanetary propagation of flare-associated energetic particles (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A propagation model which combines a Gaussian profile for particle release from the sun, with interplanetary particle densities predicted by focused diffusion, was proposed to explain the propagation history of flare associated energetic particles. This model, which depends on only two parameters, successfully describes the time-intensity profiles of 30 proton and electron events originating from the western hemisphere of the sun. Generally, particles are released from the sun over a finite interval. In almost all events, particle release begins at the time of flare acceleration.
    Keywords: ASTROPHYSICS
    Type: NASA-TM-79534
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 7
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    Feasibility of rocket propellant production on Mars (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: In situ production of rocket propellant to reduce landed mass requirements for Mars return missions has been investigated. The analysis has shown that a system which utilizes atmospheric carbon dioxide and soil moisture to produce liquid methane-oxygen propellant requires a landed mass which is less than half the mass of the ascent vehicle it produces.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Acta Astronautica; 5; Sept
    Format: text
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    NASA TECHNICAL REPORTS
  • 8
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    Atomic carbon emission from photodissociation of CO2 (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Atomic carbon fluorescence, C I 1561, 1657, and 1931 A, has been observed from photodissociation of CO2, and the production cross sections have been measured. A line emission source provided the primary photons at wavelengths from threshold to 420 A. The present results suggest that the excited carbon atoms are produced by total dissociation of CO2 into three atoms. The cross sections for producing the O I 1304-A fluorescence through photodissociation of CO2 are found to be less than 0.01 Mb in the wavelength region from 420 to 835 A. The present data have implications with respect to photochemical processes in the atmospheres of Mars and Venus.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 83; Oct. 1
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    NASA TECHNICAL REPORTS
  • 9
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    Carbonaceous chondritic material in the solar system (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Carbonaceous chondritic matrix material (CCMM) appears to be an important planet-forming unit in the mid-solar system, from the orbits of Mars to that of Uranus. The type specimen for CCMM is the low-temperature (400-500 K) assemblage of clay minerals, organic polymer, magnetite, and Ni-rich iron sulfides which constitutes the black, fine-grained matrix of primitive carbonaceous chondrites. Solar-system objects which appear to be partly or wholly made of CCMM are the satellites of Mars, most asteroids, interplanetary dust, and, perhaps, comets, satellites of the outer planets and the rings of Uranus. CCMM constituents probably formed by low-temperature reactions of higher-temperature condensates with the ambient solar composition gas, or in the case of the organic polymer, by reactions of gaseous species catalyzed by solids.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Naturwissenschaften; 65; 1978
    Format: text
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    NASA TECHNICAL REPORTS
  • 10
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    The velocity distribution of interstellar gas observed in strong UV absorption lines (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Observations of three strong interstellar UV absorption lines of N I (1199 A), N II (1083 A), and Si III (1206 A) in 47 stars of widely varying distance and a variety of spectral types are analyzed to obtain a velocity distribution function for the interstellar gas. A technique based on the maximum and minimum velocities observed along a line of sight is adopted because of heavy line blending, and results are discussed for both power-law and exponential distribution functions. The expected distribution of radiative-phase supernova remnants (SNRs) in the interstellar medium is calculated as a function of SNR birthrate and of the interstellar density in which they evolve. The results are combined with observed distance estimates, and it is shown that an interstellar density in excess of 0.1 per cu cm would be required to keep the SNRs sufficiently confined so that their cross sections are consistent with the observed number of components. The alternative possibility is considered that SNRs do not enter the radiative phase before escaping from the Galaxy or colliding with neighboring remnants.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 223
    Format: text
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