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  • 1
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    A Team Approach to the Development of Gamma Ray and x Ray Remote Sensing and in Situ Spectroscopy for Planetary Exploration Missions (1993)
    In:  CASI
    Details
    Publication Date: 2014-09-04
    Description: An important part of the investigation of planetary origin and evolution is the determination of the surface composition of planets, comets, and asteroids. Measurements of discrete line X-ray and gamma ray emissions from condensed bodies in space can be used to obtain both qualitative and quantitative elemental composition information. The Planetary Instrumentation Definition and Development Program (PIDDP) X-Ray/Gamma Ray Team has been established to develop remote sensing and in situ technologies for future planetary exploration missions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Workshop on Advanced Technologies for Planetary Instruments, Part 1; p 26
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  • 2
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    Orbital chemistry - Lunar surface analysis from the X-ray and gamma ray remote sensing experiments (1977)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: The X-ray and gamma-ray lunar surface remote sensing experiments conducted by the Apollo 15 and 16 are discussed. The data indicate mare basins that are extensively basaltic and highlands of aluminum-rich anorthositic-type feldspar. An east-west asymmetry involving higher Al/Si ratios toward the east is noted; high concentrations of a KREEP-type component along the Imbrium-Procellarum edges and throughout the basin are also observed. Lunar K/Th ratios, lowest in areas of the Imbrium and higher in the surrounding mare and highlands, may lend support to the picture of the moon as a high-temperature condensate.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Physics and Chemistry of the Earth; 10; 1, 19; 1977
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  • 3
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    Martian volatiles determined using the Mars observer gamma ray spectrometer (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: The relative abundances of H2O and CO2 and their latitude, longitude, and depth profiles on Mars sensitively reflect, as well as help control, past and present Martian climate patterns. Seasonal variations of their distributions at high latitudes also reflect and help control global weather patterns and erosion through surface weathering. A combined analysis of gamma ray line and neutron flux maps constructed from data measured using the Mars Observer Gamma Ray Spectrometer (MOGRS) should allow a determination of seasonal changes in both the horizontal and vertical structure of CO2 ice that covers the north polar cap during winter and the south polar cap throughout the year and both the horizontal and vertical structure of residual H2O ice within the top meter of the surface that was predicted from Viking observations to exist primarily at high latitudes. Particularly important in this regard will be maps of thermal and epithermal neutron fluxes measured using the MOGRS anticoincidence shield, the intensity of the hydrogen, neutron capture gamma ray line at 2.223 MeV, the intensity of a capture gamma ray line as 1.725 MeV from iron, and the intensity of an inelastic scatter gamma ray line as 1.779 MeV from silicon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Workshop on the Polar Regions of Mars: Geology, Glaciology, and Climate History, Part 1; p 8
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  • 4
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    Surface chemistry of selected lunar regions (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A completely new analysis has been carried out on the data from the Apollo 15 and 16 gamma ray spectrometer experiments. The components of the continuum background have been estimated. The elements Th, K, Fe and Mg give useful results; results for Ti are significant only for a few high Ti regions. Errors are given, and the results are checked by other methods. Concentrations are reported for about sixty lunar regions; the ground track has been subdivided in various ways. The borders of the maria seem well-defined chemically, while the distribution of KREEP is broad. This wide distribution requires emplacement of KREEP before the era of mare formation. Its high concentration in western mare soils seems to require major vertical mixing.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-X-71157 , X-682-76-149
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  • 5
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    Imaging of lunar surface chemistry from orbital X-ray data (1977)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Color images of the lunar surface from 20 deg W to 120 deg E were prepared which map the variations in the distribution of Al, Mg, and Si as expressed by the ratios of the Al/Si and the Mg/Al fluorescent X-ray intensities. Through the use of image enhancement techniques developed for the La Jolla Consortium on remote sensing of the moon, detailed information previously unobserved has been made available. The frequency distribution of the Apollo 15 and 16 intensity ratios for individual 0.25 x 0.25 deg surface units is clearly bimodal, peaking at 0.81 for mare material and 1.12 for nearside highland material, which values correspond to concentration ratios of 0.39 and 0.54, respectively, for Al/Si.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 14, 1977 - Mar 18, 1977; Houston, TX
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  • 6
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    Lunar elemental analysis obtained from the Apollo gamma-ray and X-ray remote sensing experiment (1974)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: Gamma ray and X-ray spectrometers carried in the service module of the Apollo 15 and 16 spacecraft were employed for compositional mapping of the lunar surface. The measurements involved the observation of the intensity and characteristics energy distribution of gamma rays and X-rays emitted from the lunar surface. A large scale compositional map of over 10 percent of the lunar surface was obtained from an analysis of the observed spectra. The objective of the X-ray experiment was to measure the K spectral lines from Mg, Al, and Si. Spectra were obtained and the data were reduced to Al/Si and Mg/Si intensity ratios and ultimately to chemical ratios. The objective of the gamma-ray experiment was to measure the natural and cosmic ray induced activity emission spectrum. At this time, the elemental abundances for Th, U, K, Fe, Ti, Si, and O have been determined over a number of major lunar regions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-TM-X-72195 , REPT-224 , Sov.-Am. Conf. on the Cosmochem. of the Moon and Planets; Jun 04, 1974 - Jun 08, 1974; Moscow; Soviet Union
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  • 7
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    The application of trend surface analysis to a portion of the Apollo 15 X-ray fluorescence data (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The present work discusses some useful techniques for the detailed chemical mapping of the lunar surface from X-ray fluorescence data, using Al/Si and Mg/Si intensity ratios and preliminary geologic interpretations of some relatively small lunar physiographic features. It is shown that these features can be distinguished as anomalies by employing trend surface analysis on the data. Some correlations between albedo differences and elemental ratios can be found within mare areas. A useful lower limit of 16 seconds is established for time integrals of Al/Si intensity ratios. It was not possible here to determine the minimum time integration necessary for the best spatial mapping of the Mg/Si data.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 18, 1974 - Mar 22, 1974; Houston, TX
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  • 8
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    Element concentrations from lunar orbital gamma-ray measurements (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: We report the concentrations of Th, K, Fe, Mg, and Ti in 28 geographic regions overflown by the Apollo 15 and 16 spacecraft, as determined by gamma-ray spectrometry. The observed chemical compositions are consistent with ground truth, and the two missions give reasonable agreement in a region observed by both. The chemical compositions observed require a more complex model for interpretation than the previously reported radioactivity maps. Both highlands and maria show significant variations in composition. The van de Graaff region is unique; it may possibly be the source region for 'granitic' materials such as rock 12013.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 18, 1974 - Mar 22, 1974; Houston, TX
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  • 9
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    Surface chemistry of selected lunar regions (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: A completely new analysis has been carried out on the data from the Apollo 15 and 16 gamma-ray spectrometer experiments. The components of the continuum background have been estimated. The elements Th, K, Fe, and Mg give useful results; for Ti are significant only for a few high-Ti regions. Errors are given, and the results are checked by other methods. Concentrations are reported for about 60 lunar regions; the ground track has been subdivided in various ways. The borders of the maria seem well-defined chemically, while the distribution of KREEP is broad. This wide distribution requires emplacement of KREEP before the era of mare formation. Its high concentration in western mare soils seems to require major vertical mixing.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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  • 10
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    Analysis of Phobos mission gamma ray spectra from Mars (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The determination of the elemental composition of the surface of a planetary body can be achieved, in many cases, by remote-sensing gamma ray spectroscopy. A gamma ray spectrometer was carried on the Soviet spacecraft Phobos-2, and obtained data while in an elliptical orbit around Mars. Results of two independent approaches to data analysis, one by the Soviet group and one by an American group are reported. The results for five elements are given for two different orbits of Mars. Major geologic units that contribute to the signal for each orbit have been identified. The results from the two techniques are in general agreement and there appear to be no geologically significant differences between the results for each orbit.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 18, 1991 - Mar 22, 1991; Houston, TX; United States
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