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  • LUNAR AND PLANETARY EXPLORATION  (715)
  • 1985-1989  (715)
  • 1980-1984
  • 1985  (715)
  • 201
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    Conjecture on superrotation in planetary atmospheres - A diffusion model with mixing length theory (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The component of rigid shell superrotation on Venus is discussed in the context of comparative planetary atmospheres. A simplified, heuristic analysis, utilizing mixed length theory to describe the small scale nonlinear advections of energy and angular momentum, thereby providing a closure of the dynamic system, is presented, on the basis of which a crude estimate of zonal velocity is made. The rigid shell (global average) component on Venus was calculated to be 105 m/sec.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Advances in Space Research (ISSN 0273-1177); 5; 9, 19
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  • 202
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    Temperature structure and dynamics of the middle atmosphere of Venus (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Data obtained by the Pioneer Venus Orbiter Infrared Radiometer in late 1978 and early 1979 are presented in tabular form, including, in particular, the mean temperature structure, with complete latitudinal and longitudinal coverage, and zonal-mean cloud properties. The mean thermal and cloud structures can be interpreted in terms of general circulation of the middle atmosphere. The interim results indicate that (1) the zonal winds on Venus fall to very low values above 90 km, (2) there is a strong midlatitude jet which circles the planet approximately every two days, and (3) the observed solar tides are dominated by the semidiurnal component.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Advances in Space Research (ISSN 0273-1177); 5; 9, 19
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  • 203
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    Selection of the Apollo 15 landing site (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Telescopic studies in the early 1960's pinpointed the future Apollo 15 landing site as a potential exploration site because it included one of the largest lunar sinuous rilles, Rima Hadley, and some of the highest mountains, Montes Apenninus. Additional targets were identified once Apennine-Hadley emerged as a potential landing site. Site selection processes were discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunary and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 73-75
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  • 204
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    Geologic setting of the Apollo 15 landing site (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Returned Apollo 15 samples were used to provide a remarkably comprehensive sampling of the Moon's profile and geologic history. The geological structure of the Apennine Bench Formation is described. The large collection of pigeonite and olivine basalts from the landing sites were viewed in the context of the site's geology.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunary and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 68-72
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  • 205
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    The origin of pristine KREEP: Effects of mixing between ur KREEP and the magmas parental to the MG-rich cumulates (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The magnesium/incompatible elements paradox is explained by a model that considers not only the magmasphere, but also its aftermath. A systematic mixing of primitive magnesium rich material with residual liquid is discussed as a method to account for the paradox that KREEP basalts, despite their high incompatible element contents, have moderate magnesium ratios. The KREEP basalts are compared with mare basalts.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunary and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 65-67
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  • 206
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    Some observations on the geology of the Apollo 15 landing site (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: High resolution (panoramic) and high geometric fidelity (metric) photos were taken from orbit of the lunar landing sites. Gamma ray and X-ray fluorescence spectroscopic measurement were taken to determine regional chemical composition of the Moon. Distinctive features of the Apennine Bench Formation are described. The structurally controlled topography of the Apennine Bench Formation is suggested of a lava channel or collapsed lava tube.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 60-64
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  • 207
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    The materials and formation of the imbrium basin (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The deposits around the Imbrium basin form a widespread stratigraphic datum, to which other lunar geological units may be relatively dated. More importantly, as a relatively well preserved multi-ring basin, Imbrium provides an important target of geologic investigation to study the processes involved in lunar basin formation and evolution. Two Apollo missions (Apollo 14 and 15) were send to landing sites chosen specifically to address problems of the Imbrium basin geology. Data about the deposits of the Imbrium basin are reviewed. Formational mechanics of lunar basins in general and the relations of materials collected at the highlands adjacent to the Apollo 15 landing site to Imbrium and other basins are examined.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 52-56
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  • 208
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    Apollo 15 regolith breccias and soils: Comparative petrology and chemistry (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Soils and regolith breccias contain clues to the geologic processes that contributed to the evolution of the local regolith over time. A suite of ten regolith breccias from the Apollo 15 site were compared with the results of previous studies in order to learn more about the regolith evolution at that site.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 49-51
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  • 209
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    The Apennine Bench Formation revisited (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The Apennine Bench Formation consists of pre-mare light plains materials that crop out south of the crater Archimedes, inside the Imbrium basin. This material was ascribed to either impact or volcanic origins. The characteristics of Apollo 15 KREEP basalts and the Apennine Bench Formation are reviewed to determine whether their characteristics are compatible with a volcanic origin.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 57-59
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  • 210
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    Apollo 15 mare basalts: A diverse suite or two distinct groups? (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The literature geochemical data for 60 Apollo 15 mare basalts were compiled in order to evaluate possible intra-group relationships of the Apollo 15 mare basalts. The effects of olivine or pigeonite fractionation were discussed. Models were developed to explain the trace element characteristics of the samples.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 46-48
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  • 211
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    Samples at the Apollo 15 landing site: Types and distribution (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Samples, consisting of more than 350 individually numbered samples of rock and regolith, were collected during the three EVAs on the Apollo 15 mission. Samples consisted of rock specimens, and scooped, trenched, and cored regolith samples. Petrographic and chemical analysis are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 41-45
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  • 212
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    Spectral reflectance study of the Hadley-Appenine (Apollo 15) region (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Twenty-three near infrared spectra were obtained from the Mauna Kea Observatory 2.2 m telescope. Results of an analysis of near infrared spectra obtained for surface units in the Hadley-Apennine region were presented. Compositional trends from the interior to exterior of the Imbrium are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 38-40
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  • 213
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    Ultramafic parent magmas for mare basalts? (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Solidification products of basaltic magmas (fine grained basalts and ultramafic glasses) at the Apollo 15 site were examined. Consideration of simple MgO-6IO2-Al2O3 systematics plus results of calculations of fractional crystallization was reviewed. Suggestions are presented to account for the lack of correlation between the ultramafic glasses and basalts.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 35-37
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  • 214
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    Petrology and geochemistry of highlands samples from the Apennine Front (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Individual rocks from the Hadley Delta massif, part of the Apennine Front, are described beginning with the simplest samples to the most complex breccias. Relationship among the samples were evaluated. Geological interpretations of the samples were speculative because of the limited data set, but provided models to be tested when additional data are available.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 30-34
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  • 215
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    Chemical components of the Apollo 15 regolith (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The lunar regolith is a complex mixture of many components. Compositional data is used to identify and estimate the relative importance of the various chemical components of the regolith. The results and conclusions of four methods that were applied to Apollo 15 regolith data were reviewed to determine the important chemical components: graphical techniques, analysis of individual soil particles, factor analysis, and multicomponent mixing models. This synthesis relies heavily on data and conclusions from the literature as well as new analyses on 28 regolith breccia samples, 28 soil samples, and 50 individual 1 to 2 mm particles from soil 15272.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 25-29
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  • 216
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    The geologic history of quartz-normative and olivine-normative basalts in the vicinity of Hadley Rille (Apollo 15) (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The geologic history of the quartz normative (QNB) and olivine normative (ONB) basalt types at Hadley Rille are discussed. A model for the geology of the mare basalts was constructed from a combination of field observations, sample chemistry, sample petrology and personal bias from terrestrial experience. The model proposes that the QNBs are the only mare lava type that is present as outcrop in the area traversed by the astronauts during the Apollo 15 mission. The returned QNB samples formed during a single eruptive phase of the Hadley Rille lava tube system. The ONB lavas are an exotic component transported to the site by a cratering event, or the ONBs are samples excavated from older are bedrock that was partly covered by the QNB lavas.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 22-24
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  • 217
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    Apollo 15 mare volcanism: Constraints and problems (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The Apollo 15 landing site contains more volcanics in the form of crystalline basalts and pristine glasses, which form the framework for all models dealing with the mantle beneath that site. Major issues on the petrology of the mare source regions beneath that portion of Mare Imbrium are summarized.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 13-17
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  • 218
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    Hadley Rille, lava tubes and mare volcanism at the Apollo 15 site (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Hadley Rille appears to be a collapsed lava tube/channel, whose formation history may be more intimately related to the mare units sampled at 15 than was previously thought. More work is needed relating samples and observations from Apollo 15 to the rille and its geologic evolution. As the only sinuous rille visited during the Apollo missions, Hadley Rille represents a data source that is directly applicable to the deciphering of processes involved in lunar mare volcanism.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 18-21
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  • 219
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    Extraction of information from major element chemical analyses of lunar basalts (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Major element chemical analyses often form the framework within which similarities and differences of analyzed specimens are noted and used to propose or devise models. When percentages are formed the ratios of pairs of components are preserved whereas many familiar statistical and geometrical descriptors are likely to exhibit major changes. This ratio preserving aspect forms the basis for a proposed framework. An analysis of compositional variability within the data set of 42 major element analyses of lunar reference samples was selected to investigate this proposal.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 10-12
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  • 220
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    Comparison of petrology, grain sizes and surface maturity parameters for Apollo 15 regolith breccias and soils (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: A total of 28 Apollo 15 regolith breccias were analyzed for their petrographic and textural properties and for the surface exposure indices solar noble gases and I (sub s)/Fe 0. Similarities and differences in compositional components and irradiation history were examined between regolith breccias and local, present day soils.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on tyhe Geology and Petrology of the Apollo 15 Landing Site; p 7-9
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  • 221
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    Apollo 15 mare units and their petrogenesis (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Samples from 12 different mare sites were identified and classified among the Apollo 15 samples. The genesis of the Apollo 15 mare units is summarized given the general model of mare basalt source regions and of more basalt genesis derived from a synthesis of the major oxide/major mineral, compatible siderophile, and incompatible trace element data and isotopic ratios of the Rb/Sr and Sm/Nd systems.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 4-6
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  • 222
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    Regolith erosion and regolith mixing at the Apollo 15 site on the moon (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Regolith samples from the Apollo 15 landing site were used to trace soil mixing. Mixing model calculations were performed on the chemical compositions of soils from different stations. The model was constructed using modal abundance data on crystalline fragments and green glass spherules.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Papers Presented to the Workshop on the Geology and Petrology of the Apollo 15 Landing Site; p 1-3
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  • 223
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    High stress shallow moonquakes - Evidence for an initially totally molten moon (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Thermoelastic stress calculations show that if the moon was initially molten only in the outer few hundred kilometers, as in the magma ocean model of the moon, the highlands crust should be aseismic. In contrast, if the moon was initially totally molten, high stress (1 to more than about 3 kbar), shallow (0 to about 6 km deep), compressional moonquakes should be occurring in the highlands crust. Calculations of the minimum stress drops made for the 28 observed shallow moonquakes suggest that 3 of them probably have stress drops in the kbar range. Thus, these very limited seismic data are consistent with the model that the moon was initially totally molten.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Earth and Planetary Science Letters (ISSN 0012-821X); 74; 2-3,; 149-154
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  • 224
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    Electron densities and temperatures in the Venus ionosphere Effects of solar EUV, solar wind pressure and magnetic field (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The Venus ionosphere is influenced by variations in both solar EUV flux and solar wind conditions. On the dayside the location of the topside of the ionosphere, the ionopause, is controlled by solar wind dynamic pressure. Within the dayside ionosphere, however, electron density is affected mainly by solar EUV variations, and is relatively unaffected by solar wind variations and associated magnetic fields induced within the ionosphere. The existence of a substantial nightside ionosphere of Venus is thought to be due to the rapid nightward transport of dayside ionospheric plasma across the terminator. Typical solar wind conditions do not strongly affect this transport and consequently have little direct influence on nightside ionospheric conditions, except on occasions of extremely high solar wind dynamic pressure. However, both nightside electron density and temperature are affected by the presence of magnetic field, as in the case of ionospheric holes.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Advances in Space Research (ISSN 0273-1177); 5; 4, 19; 313-316
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  • 225
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    Interaction of Titan's atmosphere with Saturn's magnetosphere (1985)
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    Publication Date: 2011-08-19
    Description: The Voyager 1 measurements made during the Titan flyby reveal that Saturn's rotating magnetospheric plasma interacts directly with Titan's neutral atmosphere and ionosphere. This results from the lack of an intrinsic magnetic field at Titan. The interaction induces a magnetosphere which deflects the flowing plasma around Titan and forms a plasma wake downstream. Within the tail of the induced magnetosphere, ions of ionospheric origin flow away from Titan. Just outside Titan's magnetosphere, a substantial ion-exosphere forms from an extensive hydrogen-nitrogen exosphere. The exospheric ions are picked up and carried downstream into the wake by the plasma flowing around Titan. Mass loading produced by the addition of exospheric ions slows the wake plasma down considerably in the vicinity of the magnetopause.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Advances in Space Research (ISSN 0273-1177); 5; 4, 19
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  • 226
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    Uranium distribution and 'excessive' U-He ages in iron meteoritic troilite (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Fission tracking techniques were used to measure the uranium distribution in meteoritic troilite and graphite. The obtained fission tracking data showed a heterogeneous distribution of tracks with a significant portion of track density present in the form of uranium clusters at least 10 microns in size. The matrix containing the clusters was also heterogeneous in composition with U concentrations of about 0.2-4.7 ppb. U/He ages could not be estimated on the basis of the heterogeneous U distributions, so previously reported estimates of U/He ages in the presolar range are probably invalid.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Meteoritics (ISSN 0026-1114); 20; 37-41
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  • 227
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    Differential rotation of the magnetic fields of gaseous planets (1985)
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    Publication Date: 2011-08-19
    Description: The differential rotation of the magnetic fields of Jupiter and Saturn, as well as those of Uranus and Neptune if they have internal dynamo-generated magnetic fields, is examined. It is shown that the behavior of the magnetic fields is more analogous to the sun then to the earth. Evidence is presented to support the hypothesis that polar magnetic features on Jupiter and Saturn spin more slowly than the equatorial magnetic field. Consideration is given to Jovian narrow-band kilometric radio emission, to brightness periodicities in the Io torus, and to Saturn cloud motions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geophysical Research Letters (ISSN 0094-8276); 12; 299-302
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  • 228
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    Chronology and petrogenesis of a 1.8 g lunar granitic clast:14321,1062 (1985)
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    Publication Date: 2011-08-19
    Description: Geochronological, isotopic, and trace element data for a pristine granite clast from Apollo 14 breccia 14321 obtained using Rb-Sr, Sm-Nd, and (Ar-39)-(Ar-40) methods are presented. Trace element data for a possibly related evolved rock, the quartz-monodiorite clast from breccia 15404 are also presented, and the relationship between these two rock types is discussed. The concordancy of the Rb-Sr and Sm-Nd internal isochron ages and especially the Rb-Sr model age strongly suggest that the granite clast formed 4.1 AE ago. It probably crystallized slowly in the crust and was later excavated and brecciated about 3.88 AE ago, as indicated by the Ar-Ar age. A two-stage model involving crystal fractionation followed by silicate liquid immiscibility is proposed for the lunar granite genesis.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geochimica et Cosmochimica Acta (ISSN 0016-7037); 49; 411-426
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  • 229
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    Transport of Venusian rolling 'stones' by wind? (1985)
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    Publication Date: 2011-08-19
    Description: Simulations of Venusian wind processes are described which show that particles are moved by 'rolling' at wind speeds as much as 30 percent lower than those required for saltation threshold. This mode of wind transport is only observed for sustained periods in water on earth; thus, there are similarities between aqueous fluid transport on earth and atmospheric transport on Venus. The formation of small sand ridges and grooves oriented parallel to the wind direction is associated with the rolling of grains in Venusian simulations and these structures may be unique aeolian features on Venus.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Nature (ISSN 0028-0836); 313; 771-773
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  • 230
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    Ringed planets - Still mysterious. II (1985)
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    Publication Date: 2011-08-19
    Description: The morphology of the rings of Saturn and the mechanisms proposed to explain their fluctuations and origin are discussed and illustrated with photographs and diagrams in a general review. The kinks and braids of the F ring are attributed to the gravitational effects of the known shepherding satellites and/or a number of as yet unseen moonlets; the irregular gaps in the B and inner A rings, to particle interactions (diffusion-instability processes); and the flickering spokes of the central B ring, to the rotation of the Saturn magnetic field. It is pointed out that the composition of the single Jovian ring and of the Jovian satellites can be explained if both are remnants of the planet's primordial disk, but that the rock-ice compositions of the rings and inner satellites of Saturn require a more sophisticated model, perhaps involving meteoroid erosion. The rings of Uranus and Neptune are briefly considered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Sky and Telescope (ISSN 0037-6604); 69; 19-23
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  • 231
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    Dating Archean zircon by ion microprobe: New light on an old problem (1985)
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    Publication Date: 2011-08-19
    Description: Ion microprobe analysis of zircons from three sites (Watersmeet Dome in northern Michigan, Mount Sones in eastern Antarctica, and Mount Narryer in western Australia) is discussed. Implications of the results to Archean geochronology and early Earth crust composition are addressed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 84-86
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  • 232
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    Earth's primordial differentiation, and its after-effects (1985)
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    Publication Date: 2011-08-19
    Description: The case for massive primordial melting on the Earth is circumstantial (i.e., based mainly on lunar evidence), but nonetheless compelling. The term magma ocean is probably a hyperbole. Among other things, ocean implies the system is virtually 100% liquid, with a mainly gas/liquid upper surface, and a water like viscosity of the order .01 poise. The preferred term for this phenomenon is magmasphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 79-81
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    The Aravalli sequence of Rajasthan, India: A Precambrian continental margin? (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The extent to which plate tectonics in its present form operated during the Precambrian is unknown, but is a subject of considerable current interest. A remarkable succession of Precambrian rocks in Rajasthan, Northwestern India, which may help to shed more light on this question are discussed. Data indicates that the Aravalli sequence has a number of characteristics generally ascribed to active continental margins. Although much more work is required to bear this out, the evidence suggests that the processes operating in such an environment in the early Proterozoic or late Archean were not vastly different from today.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 57-58
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    A review of noble gas geochemistry in relation to early Earth history (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: One of the most fundamental noble gas constraints on early Earth history is derived from isotopic differences in (129)Xe/(130)Xe between various terrestrial materials. The short half life (17 m.y.) of extinct (129I, parent of (129)Xe, means that these differences must have been produced within the first 100 m.y. after terrestrial accretion. The identification of large anomalies in (129)Xe/(130)Xe in mid ocean ridge basalts (MORB), with respect to atmospheric xenon, suggests that the atmosphere and upper mantle have remained separate since that time. This alone is a very strong argument for early catastrophic degassing, which would be consistent with an early fractionation resulting in core formation. However, noble gas isotopic systematics of oceanic basalts show that the mantle cannot necessarily be regarded as a homogeneous system, since there are significant variations in (3)He/(4)He, (40)Ar/(36)Ar, and (129)Xe/(130)Xe. Therefore, the early degassing cannot be considered to have acted on the whole mantle. The specific mechanisms of degassing, in particular the thickness and growth of the early crust, is an important variable in understanding present day noble gas inventories. Another constraint can be obtained from rocks that are thought to be derived from near the lithosphere asthenosphere boundary: ultramafic xenoliths.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 50
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    Hydrothermal alteration in the 3.5 b.y. old Onverwacht Group of South Africa (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: K-Ar studies of authigenic and alteration phases from the 3.5 b.y. old Onverwacht group of South Africa delineate hydrothermal metamorphism that ended 3.3 b.y. years ago. A whole rock K-Ar errochron from analysis of barite, dolomite, chert, and serpentinite (komatiite) gives an age of 3.3 b.y. with an intercept of 1,678 + or - 103. The 3.3. b.y. age for the metamorphism in the Onverwacht was confirmed by the Argon isotopes stepwise heating experiments of komatiites and basaltic komatiites from the Onverwacht Group. In addition, the errochron suggests all the phase studied equilibrated with a reservoir of hydrothermal argon with relatively uniform isotopic composition. The concept of hydrothermal activity in the Onverwacht Group is discussed and illustrated with photographs.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 25-27
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    Early evolution of the crust-mantle system (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Nd isotopic data indicate that most Archean igneous rocks including compositions ranging from komatiite to tonalite are derived from undepleted or depleted upper mantle sources. If sampling is representative, only a few require enriched sources. A major unresolved question is the fate of the material removed from the upper mantle leaving early depleted sources as residue. One possibility is that widespread depletion of the early mantle resulted from a period of early degassing and magmatism. Rare gas isotopic data, in particular 129Xe/130Xe ratios, seem to demand that the upper mantle was extensively degassed at or before 4.4 b.y. and this led to rapid growth of the atmosphere and oceans. The lower mantle, however, was not significantly degassed during this event. It is likely that such widespread degassing and magmatism of the upper mantle transferred significant quantities of incompatible elements into the uppermost mantle or crust. Once formed, such an enriched fraction should resist recycling into the mantle and collect at or near the Earth's surface. One possibility is that it collects chiefly in a zone of partial melting, analogous to the present low-velocity zone at the base of the lithosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 14-16
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    The composition of the primitive atmosphere and the synthesis of organic compounds on the early Earth (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The generally accepted theory for the origin of life on the Earth requires that a large variety of organic compounds be present to form the first living organisms and to provide the energy sources for primitive life either directly or through various fermentation reactions. This can provide a strong constraint on discussions of the formation of the Earth and on the composition of the primitive atmosphere. In order for substantial amounts of organic compounds to have been present on the prebiological Earth, certain conditions must have existed. There is a large body of literature on the prebiotic synthesis of organic compounds in various postulated atmospheres. In this mixture of abiotically synthesized organic compounds, the amino acids are of special interest since they are utilized by modern organisms to synthesize structural materials and a large array of catalytic peptides.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 8-10
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  • 238
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    The relation between the age of the subconducting slab and the recycling of sediments into the mantle (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The recycling of sediments into the mantle has become an important issue because recent papers have suggested that the geochemical inverse models of the evolution of radiogenic isotope abundances over the history of the Earth have nonunique solutions. Both the recycling of continent-derived sediments into the mantle and mixing in the mantle could produce similar geochemical effects in the mean isotopic ratios of new igneous material emplaced in continents. Recent models of Archaean heat flow and of plate tectonics during early Earth history have demonstrated that higher internal heat production of the early Earth was mainly dissipated through a higher creation rate of oceanic lithosphere. If the seafloor creation rate was higher on the early Earth, then the residence time of any one piece of oceanic lithosphere on the surface would have been shorter. It is possible that a higher rate of recycling of oceanic lithosphere into the mantle could have resulted in some transport of sediment into the mantle.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Workshop on the Early Earth: The Interval from Accretion to the Older Archean; p 1-3
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    Interannual variability of Martian weather (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Pressure, temperature, imaging, and wind data from the Mutch Memorial Station, the Viking lander located in Mars' subtropics, are used to demonstrate the existence of two disctinct regimes of northern hemisphere winter weather on Mars. One of these regime is characterized by one or more intense global dust storms in which the optical depth reaches about 5 over most of the planet. During these events, traveling baroclinic waves of the winter hemisphere are suppressed. In the other regime, there are no global dust storms, but traveling baroclinic waves are active, and high winds associated with these storms raise large quantities of dust which remain confined to a shallow layer in the northern hemisphere. The strongest winds at the Mutch Memorial Station occur during intense storms in the latter regime.
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  • 240
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    Geology and petrology of the Apollo 15 landing site - Past, present, and future understanding (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The main objectives of the Apollo 15 lunar mission were to investigate and sample materials from the Apennine Front (expected to be Imbrium ejecta and pre-Imbrian materials), the Hadley Rille, and the mare lavas of Palus Putredinis. The Hadley Rille was found to be a collapsed lava tube or channel, and from it, many mare basalt samples were collected which form two main chemical groups of the same age (3.3 b.y.), isotopic characteristics, and rate-earth element patterns. One group, olivine-normative, contains many vescular specimens and shows an olivine fraction trend. The other group, quartz-normative, is pigeonite-phyric and contains both vitrophyric and coarse-grained samples but exhibits little fractionation. The Apennine Front samples include such highland materials as ferroan anorthosites, spinel-bearing troctolites, norites, impact melts and metamorphosed breccias. A conspicuous component of the regolith breccias is volcanic green glass. The Apennine Front is characterized by a low-KREEP composition, a composition which has never been found as a pristine igneous rock type. Another unexpected discovey was the common occurrence of 3.5 b.y. old volcanic KREEP basalts. It is concluded that all major lunar processes can be profitably studied from the samples and observations at this single location.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: EOS (ISSN 0096-3941); 66; 721
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    Observations of the J = 10 manifold of the pure rotational band of phosphine on Saturn (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Saturn was observed in the vicinity of the J = 10 manifold of the pure rotational band of phosphine on 1984 July 10 and 12 from NASA's Kuiper Airborne Observatory with the facility far-infrared cooled grating spectrometer. On each night observations of the full disk plus rings were made at 4 to 6 discrete wavelengths which selectively sampled the manifold and the adjacent continuum. The previously reported detection of this manifold is confirmed. After subtraction of the flux due to the rings, the data are compared with disk-averaged models of Saturn. It is found that PH3 must be strongly depleted above the thermal inversion (approx. 70 mbar). The best fitting models consistent with other observational constraints indicate that PH3 is significantly depleted at even deeper atmospheric levels (or = 500 mbar), implying an eddy diffusion coefficient for Saturn of 10 to the 4 cm sq/sec.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 64; 549-556
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  • 242
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    The Mars ancient cratered terrain, smooth plains boundary: Implications of Viking color data for evolution of the Amenthes Region (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The global color set compiled by the Mars Consortium was investigated. The problem of application of the martian surface color data to geologic interpretation are atmospheric contributions which increase with latitude, and the high correlation among the three color bands. In southern Amenthes the classified units show areas of possible mixing between cratered tarrain and smooth plains. It is suggested that some geologically meaningful correlation exists between surface units and the transformed color data in the Amenthes region. The knobby terrain protruding through the plains units appears to be remnants of ancient cratered terrain extending northward beneath the more youthful smooth plains.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 54-56
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    Electrolysis of simulated lunar melts (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Electrolysis of molten lunar soil or rock is examined as an attractive means of wresting useful raw materials from lunar rocks. It requires only hat to melt the soil or rock and electricity to electrolyze it, and both can be developed from solar power. The conductivities of the simple silicate diopside, Mg CaSi2O6 were measured. Iron oxide was added to determine the effect on conductivity. The iron brought about substantial electronic conduction. The conductivities of simulated lunar lavas were measured. The simulated basalt had an AC conductivity nearly a fctor of two higher than that of diopside, reflecting the basalt's slightly higher total concentration of the 2+ ions Ca, Mg, and Fe that are the dominant charge carriers. Electrolysis was shown to be about 30% efficient for the basalt composition.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 44-46
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    Mineralogical studies of lunar meteorites and their lunar analogs (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The minerology and textural properties of three lunar meteorites (Yamato 791197, ALH81005, and Yamato 82192) were analyzed and compared with lunar surface rock samples. The chemical composition and textures of pyroxene and the occurrance of glass matrices were specifically addressed. The study of glass in the lunar meteorites suggests that the glass was not produced by a meteorite impact which excavated the mass into orbit towards the Earth. The glass had been devitrified on the lunar surface before the excavation, and new glass was not produced by the last impact.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 81-83
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    Identification of the youngest meteorites and a discussion of the possibility that they came from Mars (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The shergottites are a group of basaltic meteorites which are very similar in appearance to terrestrial basalts. On the Earth basalts are formed by volcanic activity. Because the shergottites so resemble terrestrial basalts and because they are apparently very young ( 1.3 billion years), it has been inferred that they come from a large planet. Small planets and asteroids lose heat from their interiors quickly and stop producing hot basaltic liquids early in their history. It appears that gases trapped in one shergotite found in Antarctica (BETA 79001) are chemically similar to the martian atmosphere (as measured by the Viking mission). The controversial speculation that the shergotites are samples of mars is examined in detail.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 38-41
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  • 246
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    Carbon isotopes in bulk carbonaceous chondrites (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The chemical and physical processes involved in the formation of the solar system are examined. Primitive matter has been found on a microscopic scale in a variety of meteorites: fragments of small solar system bodies that were never part of a large planet. This primitive matter has, in most cases, been identified by the presence of anomalous abundances of some isotopes of the chemical elements. Of particular interest for carbon isotope studies are the primitive meteorites known as carbonaceous chondrites. Using a selective oxidation technique to sort out the carbon contained in different chemical forms (graphite, carbonates, and organic matter), four carbonaceous chondrites are analyzed. The presence of the (13) C-rich component was confirmed and additional carbon components with different, but characteristic, isotopic signatures were resolved.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 32-34
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    Nd-isotopic evidence for the origin of the Sudbury complex by meteoritic impact (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: A Neodymium isotopic investigation was undertaken in order to determine the possibility that the Sudbury geological structure in Ontario, Canada was formed by meteoritic impact. Conclusive evidence points to the melting of crustal rocks by way of meteoritic impact in the forming of the Sudbury structure.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 19-23
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    Ganymede and Callisto: Beauty is only skin deep (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Ganymede and Callisto, the two giant icy satellites of Jupiter, have very nearly the same size, composition, and location in the solar system, yet their surfaces are profoundly different. A new scenario of their geologic histories indicates that the differences may be only skin deep.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 12-14
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    Aeolian geomorphology from the global perspective (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Any planet or satellite having a dynamic atmosphere and a solid surface has the potential for experiencing aeolian (wind) processes. A survey of the Solar System shows at least four planetary objects which potentially meet these criteria: Earth, Mars, Venus, and possibly Titan, the largest satellite of Saturn. While the basic process is the same among these four objects, the movement of particles by the atmosphere, the aeolian environment is drastically different. It ranges from the hot (730 K), dense atmosphere of Venus to the extremely cold desert (218 K) environment of Mars where the atmospheric surface pressure is only approximately 7.5 mb. In considering aeolian processes in the planetary perspective, all three terrestrial planets share some common areas of attention for research, especially in regard to wind erosion and dust storms. Relevant properties of planetary objects potentially subject to aeolian processes are given in tabular form.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Goddard Space Flight Center Global Mega-Geomorphology; p 64-67
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  • 250
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    What we know about Mars (but otherwise wouldn't) if it is the shergottite parent body (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The evidence that some meteorites may actually be samples of fairly large solar system bodies, specifically the moon and the planet Mars was presented. The proposed martian meteorites, called shergottites are igneous rocks that crystallized from molten magmas. Their crystallization ages are much too young to have formed by internal melting within small asteroids, and the unusual chemical composition of gases trapped when these rocks were severely shocked matches that of the martin atmosphere measured by Viking. The implications of these samples for martian evolution was discussed and suggested, that if Mars is the shergottite parent body, the martian interior is much more like that of the earth than has been previously thought. Shergottites explain presence of small magnetic field indicate that volatileement concentratins in Mars should be similar to the Earth, and explain the great lengths of volcanic flows on the martian surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 57-58
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    Chondrule-like particles provide evidence of early Archean meteorite impacts, South Africa and western Australia (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The evolution of the Earth and the Earth crust was studied. Two layers, that contain abundant unusual spherical particles which closely resemble chondroules were identified. Chondrules occur on small quantities in lunar soil, however, they are rare in terrestrial settings. Some chondrules in meteorites were formed on the surfaces of planet sized bodies during impact events. Similar chondrule like objects are extremely rare in the younger geologic record and these abundances are unknown in ancient deposits, except in meteorites. It is suggested that a part of the Earth's terminal bombardment history, and conditions favoring chondrule formation existed on the early Earth.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 47-50
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    Occultation detection of a Neptune ring segment (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: A stellar occulation event of Neptune revealed a ring segment that was previously undetected. It appears that the object is not a complete ring, but rather a localized swarm of particles which follows a ring orbit over a limited range of longitudes. To avoid confusion with the standard use of the word ring it is suggested that the feature be called an arc. The distance of the arc zone is not precisely known because so far there has been no confirmed occultation by both an arc and the planet.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 35-37
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  • 253
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    Examination of returned solar-max surfaces for impacting orbital debris and meteoroids (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Previous theoretical studies predicted that in certain regions of earth orbit, the man-made earth orbiting debris environment will soon exceed the interplanetary meteoroid environment for sizes smaller than 1 cm. The surfaces returned from the repaired Solar Max Mission (SMM) by STS 41-C on April 12, 1984, offered an excellent opportunity to examine both the debris and meteoroid environments. To date, approximately 0.7 sq. met. of the thermal insulation and 0.05 sq. met of the aluminum louvers have been mapped by optical microscope for crater diameters larger than 40 microns. Craters larger in diameter than about 100 microns found on the initial 75 micron thick Kapton first sheet on the MEB (Main Electronics Box) blanket are actually holes and constitute perforations through that blanket. The following populations have been found to date in impact sites on these blankets: (1) meteoritic material; (2) thermal paint particles; (3) aluminum droplets; and (4) waste particles.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 42-43
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  • 254
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    Evidence in meteorites for an active early Sun (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The amounts of neon-21 found in meteorite particles indicate that the Sun experienced a period of intense solar flare activity approximately 4.5 billion years ago.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 6-8
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  • 255
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    Dust devils on Mars (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Large columns of dust have been discovered rising above plains on Mars. The storms are probably analogous to terrestrial dust devils, but their size indicates that they are more similar to tornadoes in intensity. They occur at locations where the soil has been strongly warmed by the Sun, and there the surface is smooth and fine grained. These are the same conditions that favor dust devils on Earth. Warm gas from the lowest atmospheric layer converges and rises in a thin column, with intense swirl developing at the edge of the column. In one area a mosaic of Viking images shows 97 vortices in a three day period. This represents a density of vortices of about one in each 900 square kilometers. Thus, these dust devils may be important in moving dust or starting over dust storms.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 84-85
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  • 256
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    Origin and evolution of ordinary chondrite meteorites (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The effects of heating on the chemical composition, minerology, and texture of chondrite meteorites are discussed chondrite origin and evolution. Various asteroidal and nebular heating mechanisms are considered to account meteorite compositions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 78-80
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    Origin of mesosiderites as a natural consequence of planet formation (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The mineral composition of mesosiderites is described and a theory of the origin and evolution of these meteorites is presented. It is suggested that the asteroid parent body of the mesosiderites also formed in the inner solar system, perhaps just within the orbit of Mars. As a result of close planetary encounters, some bodies that formed near Earth or Venus were gravitationally perturbed into non-circular orbits; a few such bodies passed through the mesosiderite region at high relative velocities, colliding with and destroying a few of the native asteroids. Olivine-rich silicate mantles shattered into small pieces, but the stronger metal cores remained as large fragments. Much of the debris remained in circular orbits and accreted to the basaltic regoliths of intact native asteroids at low relative velocities. The large core fragments that collided with the crust greatly enriched restricted regions of the surface in metal. These localized regions were the mesosiderite progenitors; they accounted for only about 1% of the surface area of the parent bodies.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 86-87
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    Refractory inclusions in the Ornans C30 chondrite (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Several types of metedorites contain unusual objects 10 micrometers to 2 centimeters across that are enriched in refractory elements such as calcium, aluminum and titanium. These objects, commonly known as refractory inclusions, are most abundant in the meteorites known as carbonaceous chondrites. The refractory inclusions that have been found in the Ornans metedorite, a member of a little-studied group of carbonaceous chondrites are described. Some refractory inclusions in Ornans resemble those found in other meteorites, while others are unlike any seen before. The unusual inclusions in Ornans contain minerals with extraordinary enrichments in highly refractory elements.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 15-17
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    Asteroid amphitrite: Surface composition and prospects for the possible Galileo flyby (1985)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Studies of the trajectory of the Galileo mission to Jupiter recently revealed that the spacecraft can pass close to one of the largest asteroids (#29 Amphitrite). NASA has therefore altered the mission plan of the Galileo spacecraft to include a possible close flyby of Amphitrite in early December 1986, if the condition of the spacecraft allows. If this option is actually implemented, Amphitrite will become the only asteroid for which any high-spatial resolution images and reflection spectra will be available. To evaluate the value of this data and place Amphitrite in the context of the more than 600 asteroids for which some compositional information exists. Existing data was reexamined, new telescopic spectra of Amphitrite were obtained, and simulated Galileo data sets were constructed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. 16th Lunar and Planetary Sci. Conf.; p 1-5
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  • 260
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    The atmosphere of Venus: Recent findings; Proceedings of the Workshop III of the 25th COSPAR Plenary Meeting, Graz, Austria, June 25-July 7, 1984 (1985)
    In:  Other Sources
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    Publication Date: 2016-03-09
    Description: Topics discussed include the structure and dynamics of the Venus atmosphere below 100 km, radiation and chemistry below 100 km, the neutral upper atmosphere, the ionosphere, and solar wind interaction. Papers are presented on infrared spectrometry of Venus from Venera 15 and Venera 16, recent results on the Venus atmosphere from Pioneer Venus radio occultations, absorption of solar energy and the heating rate in the atmosphere of Venus, long term changes in Venus sulfur dioxide, and mechanisms of cooling of the nightside thermosphere of Venus. Also considered are recent advances in model calculations of the Venus ionosphere, current-driven plasma instabilities and auroral-type particle acceleration at Venus, and plasma measurements in the Venus near wake.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: (ISSN 0273-1177)
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  • 261
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    Admittance functions from Venus vertical gravity and modes of topographic support (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: Two-dimensional Fourier admittance functions have been estimated for various regions of Venus, using as input the Pioneer Venus topography data and the Venus vertical gravity model of Sjogren. Model admittance functions are computed for various cases, such as lithospheric loading from above, and support from below, for comparison. These models are functions of depth of compensation, flexural rigidity, and crust and mantle densities. The long wavelength topography and gravity signals contain most of the spectral power in the Venus data, and the admittances at these wavelengths are compatible with deep compensation of surface topography.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 20
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  • 262
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    Compressional environment in the location and orientation of planetary dorsa and terrestrial earthquake fault structures (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: Lunar mare ridges are not pure compressional ridges but their locations and orientations are most likely controlled by shear zones as seen from their Riedel-shear-like arrangements. On the Moon the crustal shortening has mostly taken place within mare areas but some young terra ridges are also to be seen indicating some crustal shortening also outside mare areas. This shortening has, however, not reached the same intensity as in the case of lobate scarp overthrusts on Mercury.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 18
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  • 263
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    Geologic processes on Venus: An update (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: Studies of Venera 15 and 16 radar image and altimetry data and reevaluation of Pioneer Venus and earlier Venera data have greatly expanded the perception of the variety and complexity of geologic processes on Venus. PV data have discriminated four highland regions (each different in geomorphic appearance), a large upland rolling plains region, and smaller areas of lowland plains. Two highland volcanic centers were identified that may be presently active, as suggested by their geomorphologic appearance combined with positive gravity anomalies, lightning strike clusters, and a change in SO2 content in the upper atmosphere. Geochemical data obtained by the Venera landers have indicated that one upland area and nearby rolling plains are composed of volcanic rocks, probably basalts or syenites. New Venera radar images of the Ishtar Terra region show folded and/or faulted linear terrain and associated volcanic features that may have been deformed by both compressional and extensional forces. Lowland surfaces resemble the mare basaltic lava flows that fill basins on the Moon, Mars and Earth. Ubiquitous crater like forms may be of either volcanic or impact origin; the origin of similar lunar features was determined by the character of their ejecta deposits.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 17
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  • 264
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    Impact processes and their implications for planetary formation and early evolution (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: Small impact craters dominate the geomorphology of small planetary bodies. Even Mars has extensive impact-dominated landscapes. The regoliths of the Moon and asteroids are created and maintained by impacts. It is now widely recognized that large impacts (craters 100-1000 km in diameter) are one of the major tectonic elements in the lithospheres of bodies like the Moon, Mercury, Mars and Callisto. The multiring basins these large impacts produce sometimes extend over an entire hemisphere. Such basins may have also affected tectonics during the Earth's hadean era. Although it has long been appreciated that low velocity collisions played a major role in the accretion of planetesimals into planets, recent work indicates a far more profound role for impacts. Studies of the interaction of planetary atmospheres with large impacts, begun in an effort to define the climatological effects of the K-T impactor, suggest that impacts may remove a significant fraction of a planet's atmosphere. Such removal now offers hope of explaining the puzzling systematics of the heavy noble gases in the atmospheres of the Earth, Venus, and Mars.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 6
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  • 265
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    Noble gas patterns in the atmospheres of Mars and Earth: A comparison via the SNC meteorites (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: Noble gas and nitrogen compositions in the glassy phase of the EETA 79001 shergottite correspond closely with Viking measurements. This direct evidence for the origin of the SNC meteorites on Mars, and for trapping of an unfractionated sample of Martian atmospheric gases in the 79001 glass, provides a reasonable basis for comparing the Martian and terrestrial atmospheres with more precision than that afforded by the Viking data set. Results are that, with one exception, elemental and isotopic compositions of nonradiogenic Martian noble gases are similar to those in the Earth's atmosphere; relatively small isotopic discrepancies in Kr and perhaps Xe may be attributable to different degrees of mass fractionation of a common parent reservoir. The anomaly is in Ar composition, where Martian Ar-36/AR-38 approx. 4 is strikingly lower than the values near 5.3 that characterize both the Earth and major meteoritic gas carriers. Although a primordial Martian ratio of 5.3 could in principle be altered by some planet specific process (e.g., cosmic ray spallation of surface materials) operating over geologic time, one has not been found that works.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 2
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    Mineralogy and chemistry of the Earth (1985)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: The Earth is the prototype if not typical terrestrial planet. Ideas about the origin, evolution, structure and chemistry of the planets can be tested most thoroughly on the Earth. Similarly, the study of the other planets has generated new ideas which may be applicable to the Earth. For example the concepts of magma oceans, large polar wander, global stress fields, buoyant lithosphere, deep cumulate reservoirs, multiple tectonic styles and crust generation may also apply to the Earth, present or past. It is no longer valid to think of the mantle as an essentially homogeneous undifferentiated shell of olivine with pockes of basalt providing melts to midocean ridges and oceanic islands. It appears to be a well differentiated, outgassed body with both radial and lateral chemical variations. The lower mantle is close to chondritic in its major element chemistry. The transition region is garnet and clinopyroxene rich and may be a major basalt reservoir. This would explain the thin crust paradox. Chemical stratification of the Earth probably occurred during accretion.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 14
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    Oxidation states of iron in the terrestrial planets: Evidence and implications for accretion models (1985)
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    Publication Date: 2019-01-25
    Description: Analyses of Mars spectra reveal that primary minerals may be more iron rich than average basalts on Earth, and the oxidation state of iron in the pyroxines suggests equally high or higher oxygen fugacities on Mars than Earth. Analysis of Mercury spectra reveal that silicate iron contents are substantially lower than those on Mars. Mercury, however, probably has a substantial iron core. This is consistent with a lower oxidation state of iron on Mercury than on Mars. These findings are consistent with predictions of models of equilibrium condensation and homogeneous accretion. Those models predict that Mercury would have negligible Fe(2+) in silicates (Fe/Fe+Mg approx. 0.5). For Mercury iron should be virtually all metallic, while for Mars the iron would be all oxidized as FeS and silicate. Surface measurements of Fe/Fe+Mg on Venus, Earth, and Mars further support the predicted relative increase in Fe/Fe+Mg ratio (increased oxidation state) with distance from the Sun. The implied high oxygen fugacities on Mars (Fe(3+) in silicates) provide additional consistence with the model predictions.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 3
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    Relationships between chondritic meteorites and planets (1985)
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    Publication Date: 2019-01-25
    Description: Chondrites formed in the solar nebula prior to the formation of planets; they probably constituted the bulk of preplanetary solids in the inner solar system. In the highly reduced enstatite chondrites 10% of Si is metallic; in the highly oxidized CM and CI chondrites 20-30% of Fe is in the +3 state. The high density of Mercury implies that nebular Fe was reduced, whereas the low density of Mars indicates that a large fraction was oxidized. Most rare gases in the terrestrial planets seem to have accreted trapped in grains; Venusian interelement ratios resemble those in enstatite chondrites; Earth and Mars ratios are more like those in ordinary or carbonaceous chondrites. These observations imply that enstatite chondrites formed near the Sun (near Venus?), the carbonaceous chondrites formed far from the Sun, the ordinary chondrites at an intermediate location. Compositional data on Mercury, comets, an asteroidal fragment, and the moons of Mars are badly needed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 1
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  • 269
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    Noble gases in meteorites and terrestrial planets (1985)
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    Publication Date: 2019-01-25
    Description: Terrestrial planets and chondrites have noble gas platforms that are sufficiently alike, especially Ne/Ar, that they may have acquired their noble gases by similar processes. Meteorites presumably obtained their noble gases during formation in the solar nebula. Adsorption onto C - the major gas carrier in chondrites - is the likely mechanism for trapping noble gases; recent laboratory simulations support this hypothesis. The story is more complex for planets. An attractive possibility is that the planets acquired their noble gases in a late accreting veneer of chondritic material. In chondrites, noble gases correlate with C, N, H, and volatile metals; by Occam's Razor, we would expect a similar coupling in planets. Indeed, the Earth's crust and mantle contain chondritic like trace volatiles and PL group metals, respectively and the Earth's oceans resemble C chondrites in their enrichment of D (8X vs 8-10X of the galactic D/H ratio). Models have been proposed to explain some of the specific noble gas patterns in planets. These include: (1) noble gases may have been directly trapped by preplanetary material instead of arriving in a veneer; (2) for Venus, irradiation of preplanetary material, followed by diffusive loss of Ne, could explain the high concentration of AR-36; (3) the Earth and Venus may have initially had similar abundances of noble gases, but the Earth lost its share during the Moon forming event; (4) noble gases could have been captured by planetestimals, possibly leading to gravitational fractionation, particularly of Xe isotopes and (5) noble gases may have been dissolved in the hot outer portion of the Earth during contact with a primordial atmosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst. Terrest. Planets: Comp. Planetology; p 1
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    Lunar and Planetary Science Conference, 16th, Houston, TX, March 11-15, 1985, Proceedings. Part 1 (1985)
    In:  Other Sources
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    Publication Date: 2016-03-09
    Description: Various papers on lunar studies, meteorites and cosmic dust, Mars, and tektites are presented. The topics discussed include: very high potassium basalt; complications in mare basalt petrogenesis; mare basalt genesis; modeling trace elements and isotopic ratios; Zr-Hf-Ta fractionation during lunar evolution; petrology of the Apollo 12 highland component; petrologic province maps of the lunar highlands derived from orbital geochemical data; petrology and chemistry of Apollo 12 regolith breccias; chemical variability and origin of agglutinitic glass; multistage exposure history of the 74261 soil constituents; and an experimental investigation of agglutinate melting mechanisms; shocked mixtures of sodium and potassium feldspars. Also addressed are: cooling history of some Antarctic ureilites; the Leoville accretionary breccia; ubiquitous brecciation after metamorphism in equilibrated ordinary chondrites; layer silicates in a chondritic porous interplanetary dust particle; estimates of rheological properties for flows on the Martian volcano Ascraeus Mons; the Martian dust storm of Sol 1742; and late Eocene North American microtektites and clinopyroxene-bearing spherules.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: (ISSN 0148-0227)
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    Lunar and Planetary Science Conference, 15th, Houston, TX, March 12-16, 1984, Proceedings. Part 2 (1985)
    In:  Other Sources
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    Publication Date: 2016-03-09
    Description: Subjects of lunar petrology are discussed, taking into account Apollo 14 aluminous mare basalts and their possible relationship to KREEP, the petrology and geochemistry of clasts from consortium breccia, the depths of the mare basalt source region, the origin of olivine at Copernicus, a transient heating event in the history of a highlands troctolite from Apollo 12 soil, and the composition and evolution of the lunar crust in the Descartes highlands. Other topics explored are related to early earth and magmatic processes, differentiated meteorites, chondritic meteorites, other planets and remote sensing, and cratering. Attention is given to the gravity field of Venus at constant altitude and comparison with earth, a spectral analog of Martian soil, dark halo craters and the thickness of grooved terrain on Ganymede, the geomorphology of Rhea, a Monte Carlo model of lunar megaregolith development, the scaling of complex craters, crustal radiogenic heat production and the selective survival of ancient continental crust, and the formation of an impact-generated H2O atmosphere and its implications for the early thermal history of the earth.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: (ISSN 0148-0227)
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    Observations of Uranus' satellites: Bibliography and literature search (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: A literature search has yielded more than 10,000 observations of the satellites of Uranus made from 1787 to 1985. The type (photographic, micrometer) and the number of observations are tabulated in 5 year increments and a complete bibliography is provided.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-176538 , JPL-PUB-85-79 , NAS 1.26:176538
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  • 273
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    Titan's organic chemistry (1985)
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    Publication Date: 2019-06-28
    Description: Voyager discovered nine simple organic molecules in the atmosphere of Titan. Complex organic solids, called tholins, produced by irradiation of the simulated Titanian atmosphere, are consistent with measured properties of Titan from ultraviolet to microwave frequencies and are the likely main constituents of the observed red aerosols. The tholins contain many of the organic building blocks central to life on earth. At least 100-m, and possibly kms thicknesses of complex organics have been produced on Titan during the age of the solar system, and may exist today as submarine deposits beneath an extensive ocean of simple hydrocarbons.
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    Lunar regolith fines - A source of hydrogen (1985)
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    Publication Date: 2019-06-28
    Description: The theoretical evaluation of the lunar regolith fines as a primary source of hydrogen reveals that a minimum order of magnitude increase in hydrogen content is possible in beneficiated fines because both particle size and particle shape play a significant role in the relationship of volume percent of surface coating to grain size. The lunar regolith fines meet the basic requirement for beneficiation because a major portion (minimum two-thirds) of the hydrogen occurs in the less than 20-micron-size fraction, a relatively small part of the fines. Beneficiation should be accomplished by a combination of vibratory screening followed by cyclone and/or possibly electrostatic separation. Early exploitation of the lunar regolith fines for hydrogen probably will be limited to hydrogen obtained as a by-product or co-product from the mining and processing for other elements or materials because a minimum of about 13,600 tons to about 19,600 tons of 100 ppm hydrogen-bearing lunar regolith fines will have to be processed with about 3,100 tons to about 4,500 tons, respectively, of concentrate heated to supply 1 ton of hydrogen, yielding a recovery of about 74 percent to about 51 percent respectively, of the hydrogen.
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    Guide to using lunar soil and simulants for experimentation (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: It is pointed out that lunar soil can be described as well-graded silty sands or sandy silts with an average particle size by weight in the range from 0.040 to 0.130 mm. The density of in situ bulk lunar soil is typically 1.4 to 1.9 g/cu cm. Changes in soil from moon to laboratory are considered along with some critical differences between simulants and lunar soil. Attention is given to agglutinates, iron metal distributed throughout the agglutinatic glass, solar wind hydrogen, and major lunar minerals (anorthite, pyroxene, ilmenite, olivine). The use of lunar fines as experimental samples is discussed, and the characteristics of simulants for experiments are examined, taking into account grain size distribution, particle type distribution, a highlands simulant, and a high titanium mare simulant. Simulants for testing equipment and structures are also described.
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  • 276
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    The next generation geophysical investigation of the moon (1985)
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    Publication Date: 2019-06-28
    Description: Planetary geophysics has mainly the objective to determine the structure, composition, and state of a given body and the relationship between internal processes and surface tectonic features. The moon represents an obvious initial case for application of geophysical techniques to bodies other than the earth. As a result of the Apollo program and associated scientific investigations, some initial progress was made toward geophysical exploration of the moon. The obtained results are briefly discussed, and some major unresolved issues are pointed out. The present status of lunar geophysical data sets is evaluated, taking into account the issues cited and the extent to which future orbital surveys and surface measurements may resolve the remaining problems. Attention is given to seismic data, electromagnetic sounding data, heat-flow data, gravity/topography data, and paleomagnetic data.
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    Geochemical and petrological sampling and studies at the first moon base (1985)
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    Publication Date: 2019-06-28
    Description: Strategic sampling appropriate to the first-order lunar base can advance a variety of first-order lunar geochemical and petrological problems. Field observation and collection of samples would be done on the lunar surface, but detailed analysis would be done mainly in terrestrial laboratories. Among the most important areas of investigation for which field observations can be made and samples can be collected at the initial base are regolith studies, studies of mare and highlands stratigraphy, and a search for rare materials such as mantle nodules. Since the range of exploration may be limited to a radius of about 20 km from the first lunar base, locating the base near a mare-highlands boundary would enable the greatest latitude in addressing these problems.
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    The need for a lunar base - Answering basic questions about planetary science (1985)
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    Publication Date: 2019-06-28
    Description: After assessing the state of current understanding of the planetological characteristics of the moon, attention is given to numerous questions that have arisen about the history of the moon and to prospective methods for their investigation through lunar exploration. One such exploratory mission will be that of the unmanned Lunar Geoscience Observer; the greatest prospects for important discoveries, however, are foreseen in manned lunar exploration. More sophisticated instruments and preliminary analyses are noted to be possible in manned exploration, although the possibility of contamination of samples is greater.
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  • 279
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    Utilizing the permafrost on Mars (1985)
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    Publication Date: 2019-06-28
    Description: It is noted that analogy between earth landforms resulting from the presence of permafrost has led to the suggestion that ground ice or water was at one time present on Mars. Only a regolith sample will confirm this. With these technologies as background, and known locations of subsurface water, development of a water supply base on Mars can then assume validity and significance. Current practices in terrestrial periglacial environments may be applicable to the Martian situation, taking into account site specific modifications of these techniques.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: AAS 84-182
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    Martian meteorology and dust storms from Viking observations (1985)
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    Publication Date: 2019-06-28
    Description: Analysis of Viking lander data on atmospheric pressure and temperature variations showed that planning for a manned base will require careful consideration of the effects of local and global dust storms. It is demonstrated that there may be preferred seasons for landing when dust storms are not at maximum strength, as well as preferred latitudes where dust storms are uncharacteristically weak. Viking I data on the diurnal variation in pressure and temperature prior to and during dust storm events are reproduced in graphic form.
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    Type: AAS 84-168
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    Geology of icy satellites (1985)
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    Publication Date: 2019-06-28
    Description: The geology of the major icy satellites of Jupiter, Saturn, Uranus, and Neptune is discussed in terms of the four major processes that shape icy satellite surfaces: impact cratering, volcanism, tectonism, and interactions with planetary magnetospheres and solar radiation. The role of these processes in creating the differences that exist among the satellites, in particular the orderly progression of geological properties in the Jovian satellites, is emphasized. Important questions left open after the Voyager missions are summarized.
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  • 282
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    The atmospheres of icy bodies (1985)
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    Publication Date: 2019-06-28
    Description: Ices are considered as the major volatile-carrying solid in the outer solar system. As such, they play a major role in forming atmospheres of icy satellites and the comas of comets and they have probably contributed to the enrichment of heavy elements in outer planet atmospheres. A possible role for clathrate hydrates in causing the activity of distant comets and sub-surface processes on icy satellites seems worthy of further study.
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  • 283
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    Evolution of Titan's coupled ocean-atmosphere system and interaction of ocean with bedrock (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: A recent model for the surface state of Titan proposes a liquid ethane-methane-molecular nitrogen layer of order one kilometer thick which because of stratospheric methane photolysis has become increasingly ethane-rich with time. The interaction of such an ocean with the underlying 'bedrock' of Titan (assumed to be water-ice or ammonia hydrate) and with the primarily nitrogen atmosphere is explored. It is concluded that although modest exchange of oceanic hydrocarbons with enclathrated methane in the bedrock can in principle occur, it is unlikely for reasonable regolith depths. The surprisingly high solubility of water-ice in liquid methane implies that topographic features on Titan of order 100 meters in height can be eroded away on a time scale of one-billion years. The large solubility difference of N2 in methane versus ethane implies that the ocean composition is a strong determinant of atmospheric pressure; a simple radiative model of the Titan atmosphere is employed to demonstrate that significant surface pressure and temperature changes can occur as the oceanic composition evolves with time.
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    Ices in planetary rings (1985)
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    Publication Date: 2019-06-28
    Description: Understanding the structure and behavior of Saturnian rings in terms of properties of ices is basic for evolutionary planetology. The available information indicates the presence of quite pure, probably amorphous water ice in the form of medium-grained frost in a fairy castle structure with a low thermal inertia. Tidal forces and interparticle collisions lead to continuous break-up and re-formation of loose aggregates of smaller particles. Micrometeoroid bombardment and proton irradiation are important for explaining the mechanical and optical properties of the surfaces of ring particles. The transfer of angular momentum and mass among the rings should homogenize the chemical and structural characteristics of the ring ices. Uranian rings may be made of carbon-covered methane ice particles.
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    Shock vaporization and the accretion of the icy satellites of Jupiter and Saturn (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The known properties of water and ice over a wide range of pressures and temperatures are applied to describe constraints on the shock vaporization processes for water and ice in the solar system. In particular, the role of impact vaporization acting during the formation of the Jovian and Saturnian satellites is examined in an attempt to explain the observed density in terms of composition of these rock and ice objects. A possible model of accretion of icy satellites is considered which predicts that the amount of ice devolatilization is related to planetary size.
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    The composition and structure of planetary rings (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The properties of planetary ring systems are summarized herein; emphasis is given to the available evidence on their compositions and to their dynamical attributes. Somewhat contaminated water ice makes up the vast expanse of Saturn's rings. Modified methane ice may comprise Uranus' rings while silicates are the likely material of the Jovian ring. Saturn's rings form an elaborate system whose characteristics are still being documented and whose nature is being unravelled following the Voyager flybys. Uranus' nine narrow bands display an intriguing dynamical structure thought to be caused by unseen shephard satellites. Jupiter's ring system is a mere wisp, probably derived as ejecta off hidden parent bodies.
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  • 287
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    Charged particle modification of ices in the Saturnian and Jovian systems (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The modification by ion bombardment of the surfaces of icy objects in the Saturnian and Jovian systems is discussed. Chemical changes in ices are induced by breaking of bonds and by implantation of incident ions. Long-term irradiation by fast ions produces physical changes such as increasing the surface reflectivity and ability to scatter light. On large satellites, molecules which are ejected by ion bombardment are redistributed across the surfaces of large satellites. For small satellites and ring particles bombarded by ions, such as those of Saturn, most or all of the sputtered material is lost to space, forming a neutral torus in the locale of the satellite orbits and rings and supplying ions to the magnetosphere. Noting the existence of such a torus, the sputter erosion and possible stabilization of the E-ring of Saturn is discussed.
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  • 288
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    Spectral properties of water ice and contaminants (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: For remote sensing studies of ices in the solar system, it is important to understand the optical properties of water ice, and mixtures of ice and particulate materials. The present paper has the objective to review the current understanding of the spectral properties of ice, and mixtures of ice and particulates. The review is to provide a basis for the understanding of the remote sensing of ice. It is found that reflectance spectra of ice-soil intimate mixtures are complex, nonlinear functions of the optical and physical properties of the components which comprise the surface.
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    Rheologies of H2O ices Ih, II, and III at high pressures - A progress report (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Ordinary hexagonal ice (ice Ih) represents the stable crystalline form of H2O on the earth's surface. It is known that ice exists elsewhere in the solar system. Thus, several of the moons of Saturn and Jupiter are composed predominately of H2O and their surface temperatures are about 75 and 100 K. The pressures in the interior of some of the larger of the moons may be as high as 3 GPa. The involved pressures and temperatures extend far beyond the conditions over which the rheological laws for ice Ih can be confidently extrapolated. It is, therefore, necessary to obtain information regarding the rheologies of H2O ices in pressure and temperature ranges which had not yet been previously considered. Since 1981, over 100 triaxial compression tests have been conducted over a wide range of temperatures (77 to 258 K) and pressures (0.1 to 350 MPa). The present paper provides a progress report of these experiments.
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  • 290
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    Clathrate hydrates in the solar system (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Clathrate hydrates are crystalline compounds in which an expanded ice lattice forms cages that contain gas molecules. There are two principal hydrate structures. Structure I, with a 12 A cubic unit cell, contains 46 water molecules and 8 cages of two types, giving an ideal formula (for CH4) of CH4.5.75H2O. The actual formula contains somewhat more water as the cages are not completely filled. Other examples that form Structure I hydrates are C2H6, C2H4, C2H2, CO2, SO2, OCS, Xe, H2S. Structure II, with a 17 A cubic unit cell, contains 136 water molecules, and 8 large and 16 small cages. The ideal formula for CHCl3 is CHCL3.17H2O. Other examples of Structure II hydrates include C3H8, C2H5Cl, acetone, and tetrahydrofuran. Small molecules such as Ar, Kr and probably N2 and O2 also form a Structure II hydrate. The small molecules occupy both the large and small cages, giving an ideal formula of Ar.5.67H2O. The conditions of pressure and temperature for hydrate formation are discussed.
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    Buoyant station mission comcepts for titan exploration (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: An advanced mission to this unique satellite of Saturn appropriate to the turn-of-the-century time period is described. The mission concept evolves about one or more buoyant stations (balloons and/or airship) operating at varying altitudes in Titan's atmosphere. An orbiter of Titan provides communications link support and accomplishes remote sensing science objectives. Use of buoyant stations are favored over a fixed site lander for two reasons: (1) adaptable to several possible surface physical states and topographies; and (2) capable of exploring both the atmosphere and surface with regional and possibly global mobility. Auxiliary payload concepts investigated include tethered packages and sounding rockets deployed from the buoyant station, and haze probes and surface penetrators deployed from the orbiter. The paper describes science objectives and payloads, propulsion system/mass delivery trades, balloon design requirements and deployment/motion characteristics, and communications link geometry and data characteristics.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: IAF PAPER 85-417
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  • 292
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    Voyager-Uranus at our doorstep (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Following the encounter of Voyager 2 with Saturn and the subsequent approach, in January 1986, to the planet Uranus, the NASA Deep Space Network (DSN) undertook a reshaping of Voyager's end-to-end data system to provide communication to earth with a sufficient number of images for Uranus characterization. In-flight evolution of the spacecraft and ground system is described, with particular attention given to the aspects of target motion compensation, line enhancement, arraying, and encoding data streams. Solutions to the on-board problems encountered during the flight are presented. Voyager and its principal elements, an actuator for the scan platform, and the coding diagram are among the illustrations included.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: IAF PAPER 85-390
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    Project Cassini - A potential collaborative ESA/NASA Saturn Orbiter and Titan Probe mission (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Project Cassini is concerned with a potential collaborative mission to Saturn and Titan. The project has been the subject of a joint ESA/NASA Technical Assessment Study from April 1984 to July 1985. The spacecraft consists of a Saturn Orbiter and a Titan entry Probe. Science objectives with respect to Titan include a determination of the abundances of atmospheric constituents and isotope ratios, a study of the distribution of trace gases, cloud physics, and a determination of the state of the surface. Other science objectives are related to Saturn, the rings, icy satellites, the magnetosphere of Saturn, and asteroids. Attention is given to mission design, the spacecraft, and future prospects.
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    Type: IAF PAPER 85-396
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    Optical observations of the AMPTE artificial comet and magnetotail barium releases (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: The first AMPTE artificial comet was observed with a low light level television camera operated aboard the NASA CV990 flying out of Moffett Field, California. The comet head, neutral cloud, and comet tail were all observed for four minutes with an unifiltered camera. Brief observations at T + 4 minutes through a 4554A Ba(+) filter confirmed the identification of the structures. The ion cloud expanded along with the neutral cloud at a rate of 2.3 km/sec (diameter) until it reached a final diameter of approx. 170 km at approx. T + 90 s. It also drifted with the neutral cloud until approx. 165 s. By T + 190 s it had reached a steady state velocity of 5.4 km/sec southward. A barium release in the magnetotail was observed from the CV990 in California, Eagle, Alaska, and Fairbanks, Alaska. Over a twenty-five minute period, the center of the barium streak drifted southward (approx. 500 m/sec), upward (24 km/sec) and eastward (approx 1 km/sec) in a nonrotating reference frame. An all-sky TV at Eagle showed a single auroral arc in the far North during this period.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-176463 , NAS 1.26:176463 , YR-1
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    Experimental investigation of crater growth dynamics (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: This work is a continuation of an ongoing program whose objective is to perform experiments and to develop scaling relationships for large-body impacts onto planetary surfaces. The centrifuge technique is used to provide experimental data for actual target materials of interest. With both power and gas guns mounted on the rotor arm, it is possible to match various dimensionless similarity parameters, which have been shown to govern the behavior of large-scale impacts. The development of the centrifuge technique has been poineered by the present investigators and is documented by numerous publications, the most recent of which are listed below. Understanding the dependence of crater size upon gravity has been shown to be key to the complete determination of the dynamic and kinematic behavior of crater formation as well as ejecta phenomena. Three unique time regimes in the formation of an impact crater have been identified.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-176392 , NAS 1.26:176392
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    A Note on Jupiter's Gossamer Ring (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: The newly discovered gossamer ring of Jupiter, composed largely of micron-sized grains, exhibits a significant peak very near the synchronous radius. It is believed that this peak is associated with an unobserved source consisting of large bodies that straddle the synchronous orbit. An alternative evolutionary mechanism is offered, which is the gyrophase drift towards the synchronous orbit, of fine grains, which necessarily are electrostatically charged within the Jovian magnetosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: California Univ., San Diego, La Jolla Trapped Particle Absorption by the Ring of Jupiter; 9 p
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    Electrons and Cosmic Ray Produced Protons in Saturn's Inner Magnetosphere (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: The Cerenkov detector on Pioneer 11 previously observed Crand protons above 600 MeV in Saturn's inner magnetosphere, mixed with a poorly understood background of energetic electrons. The electron count is separated from the proton counts and the first-order angular distributions are established for each species. To do this the theoretical relationships among the harmonic coefficients of the count rate is used as a function of spacecraft roll angle. The majority of the counts were electrons with energy above several MeV; i.e., with drift periods shorter than the satellite orbital resonance. The electrons have isotropic pitch angle distributions, and the protons pancake over most of the region between Nimas and the rings, although there is a small region of dumbbell proton distributions in the vicinity of Janus and Epimetheus.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: California Univ., San Diego, La Jolla Trapped Particle Absorption by the Ring of Jupiter; 30 p
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    Proceedings of the MECA Workshop on The Evoluation of the Martian Atmosphere (1985)
    In:  CASI
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    Publication Date: 2019-06-28
    Description: Topics addressed include: Mars' volatile budget; climatic implications of martian channels; bulk composition of Mars; accreted water inventory; evolution of CO2; dust storms; nonlinear frost albedo feedback on Mars; martian atmospheric evolution; effects of asteroidal and cometary impacts; and water exchange between the regolith and the atmosphere/cap system over obliquity timescales.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-176899 , NAS 1.26:176899 , LPI-TR-86-07
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    The Nature of Martian Flow Ejecta Craters (1985)
    In:  CASI
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    Publication Date: 2014-10-08
    Description: Ejecta with flow features and discrete termini surround many fresh Martian craters. Several morphologies of the flow-like ejecta are observed; they are found globally and in nearly all terrains. It is suggested that the morphology of flow ejecta craters is related to the amount of subsurface volatiles and/or to atmospheric drag effects. It was attempted to constrain factors which could contribute to the ejecta morphology such as latitude, elevation, and terrain unit, however, they involved only one or two constrained variables or used global data sets based on Mariner 9 information. Viking-based data sets are becoming available and may provide a better base from which an understanding of the factors which governs ejecta morphology may be obtained. Block sizes of Martian flow ejecta may provide clues to the ejecta emplacement process.
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    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984; p 202-203
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    Newly Discovered Martian Impact Basins (1985)
    In:  CASI
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    Publication Date: 2014-10-08
    Description: Three previously unrecognized Martian impact basins were discovered through detailed mapping of landforms, structures and terrains near Cassini and Al Qahira basins. Al Qahira A lies on the Martian dichotomy boundary and intersects the older basin, Al Qahira. It has four rings that are expressed by a variety of landforms. Southwestward Al Qahira A is out by a younger Basin, Al Qahira B. Al Qahira B is a highly degraded basin with one identifiable ring. Its ring is expressed by a few massifs, knobs and inward-facing scarps, but is recognized by the distributions of wrinkle ridges and plains units. Cassini A lies southward of the younger Cassini Basin and is intersected by it. It probably has four rings. The importance of detailed mapping of various types of landforms and terrains to the discovery of basins on Mars are demonstrated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984; p 200-201
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