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  • Other Sources  (1,538)
  • LUNAR AND PLANETARY EXPLORATION  (788)
  • FLUID MECHANICS AND HEAT TRANSFER  (323)
  • SPACECRAFT DESIGN, TESTING AND PERFORMANCE  (219)
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  • 1
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    (Ar-39)-(Ar-40) dating of mesosiderites - Evidence for major parent body disruption less than 4 Ga ago (1990)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The (Ar-39) (Ar-40) chronologies were determined for 14 different mesosiderites representing the full range of classification according to recrystallization, and these chronologies were compared with analogous data for other meteorite types and for lunar highland rocks. Results of Ar-Ar chronologies indicate the history of a degassing of Ar due to a major thermal event that occurred less than 3.9 Ga ago; this event is not the metal-silicate mixing event, which is known to have occurred earlier than 4.4 Ga ago. It is suggested that a major collisional disruption-reassembly event less than 3.9 Ga ago took place, leaving the metal-silicate breccias buried under tens of kilometers of rubble, where they cooled slowly through the Ar closure temperatures.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geochimica et Cosmochimica Acta (ISSN 0016-7037); 54; 2549-256
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  • 2
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    Detection of the J-10 Manifold of the Pure Rotational Band of Phosphine on Saturn (1984)
    In:  CASI
    Details
    Publication Date: 2014-09-17
    Description: The detection of the J = 10 manifold of the pure rotational band of PH3 on Saturn is reported. The observations were made from the far-infrared cooled grating spectrometer. The wavelengths and observed brightness temperatures for the full disk plus rings are 89 + or - 3 K at 97.04 micrometer, 77 + or - 3 K at 102.72 micrometer, 77 + or - 3 K at 102.94 micrometer, and 83 + or - 3 K at 105.12 micrometers. The points of 97.04 and 105.12 micrometers establish the continuum level and the two points near 103 micrometers measure the depth of the PH3 manifold. After the flux due to the rings is subtracted, the depth of the feature is 16 + or - 6 K relative to the nearby 102 K continuum. These results are compared to theoretical models which parameterize the PH3 mixing ratio as x = x sub zero (P/P sub zero)(alpha) for P P sub zero and as x = x sub zero for P or = P, where P is the total pressure and alpha = H/h is the ratio of the dynamical scale height (H) and the scale height for decreasing the PH3 mixing ratio (h). The parameters x sub zero, P sub zero, and h were varied, as well as the H/He mixing ratio and the pressure-temperature profile. The data are well fitted using pressure-temperature profiles. The preferred values of h, P sub zero, and x sub zero imply that there is little or no PH3 above the thermal inversion and that the mixing ratio below the inversion is consistent with PH3 being 1 to 4 times overabundant relative to the solar P/H ratio.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Airborne Astron. Symp.; p 76-80
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  • 3
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    A Study of Saturn's E-Ring Particles Using the Voyager 1 Plasma Wave Instrument (1993)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The flyby of Voyager 1 at Saturn resulted in the detection of a large variety of plasma waves, e.g., chorus, hiss, and electron cyclotron harmonics. Just before the outbound equator crossing, at about 6.1 R(sub s), the Voyager 1 plasma wave instrument detected a strong, well-defined low-frequency enhancement. Initially it was suggested that plasma waves might be responsible for the spectral feature but more recently dust was suggested as at least a partial contributor to the enhancement. In this report we present evidence which supports the conclusion that dust contributes to the low-frequency enhancement. A new method has been used to derive the dust impact rate. The method relies mainly on the 16-channel spectrum analyzer data. The few wide band waveform observations available (which have been used to study dust impacts during the Voyager 2 ring plane crossing) were useful for calibrating the impact rate from the spectrum analyzer data. The mass and, hence, the size of the dust particles were also obtained by analyzing the response of the plasma wave spectrum analyzer. The results show that the region sampled by Voyager 1 is populated by dust particles that have rms masses of up to few times 10(exp -11) g and sizes of up to a few microns. The dust particle number density is on the order of 10(exp -3) m(exp 3). The optical depth of the region sampled by the spacecraft is 1.04 x 10(exp -6). The particle population is centered about 2500 km south of the equatorial plane and has a north-south thickness of about 4000 km. Possible sources of these particles are the moons Enceladus and Tethys whose orbits lie within the E-ring radial extent. These results are in reasonable agreement with photometric studies and numerical simulations.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-194694 , NAS 1.26:194694 , U-OF-IOWA-93-19
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  • 4
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    The chemistry of micrometeoroids (A0187-1) (1984)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: The prime objective of this experiment is to obtain chemical analyses of a statistically significant number of micrometeoroids. These data will then be compared with the chemical composition of meteorites. Secondary objectives of the experiment relate to density, shape, mass frequency, and absolute flux of micrometeorids as deduced from detailed crater geometrics (depth) diameter, and plane shape, and number of total events observed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Langley Research Center Long Duration Exposure Facility (LDEF); p 127-130
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  • 5
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    The SCR Ne-21 and Ar-38 in lunar rock 68815: The solar proton energy spectrum over the past 2 MYR (1993)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: We determined concentration profiles of Ne-21, Ne-22, and Ar-38 produced by solar protons as a function of depth in oriented lunar rock 68815. A comparison with model predictions indicate a solar proton flux J(4(pi)(r); E greater than 10 MeV) of 100-125 p/sq. cm/s and a rigidity, R sub 0, of 85-100 MV, assuming an erosion rate of 1-2 mm/Myr. These results for 68815 and similar results on 61016 define the integrated solar proton energy spectrum at the moon over the past approximately 2 Myr.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M; p 521-522
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  • 6
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    Discovery of natural gain amplification in the 10-micrometer carbon dioxide laser bands on Mars - A natural laser (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Fully resolved intensity profiles of various lines in the carbon dioxide band at 10.4 micrometers have been measured on Mars with an infrared heterodyne spectrometer. Analysis of the line shapes shows that the Mars atmosphere exhibits positive gain in these lines. The detection of natural optical gain amplification enables identification of these lines as a definite natural laser.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science; 212; Apr. 3
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  • 7
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    The atmosphere of Jupiter - An analysis of the Voyager radio occultation measurements (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Coherently related S and X band signals of 2.3 and 8.4 GHz, respectively, which were transmitted from Voyagers 1 and 2 were used to probe the Jovian atmosphere. Height profiles of the gas refractivity, molecular number density, pressure, temperature, and microwave absorption in the troposphere and stratosphere were observed at latitudes ranging from 0 to 70 deg S. At 1000 mbar, the temperature was + or - 5 K and the lapse rate was equal to the adiabatic value of 2.1 K/km within the resolution of the measurements. The ammonia abundance in this region was 0.022 + or - 0.008%, which is in good agreement with values derived from cosmic abundance considerations. The tropopause at the 140 mbar level had a temperature of 110 K, which increased with increasing altitude, reaching 160 + or - 20 K in the 10 to 1 mbar region. Significant horizontal density variations were detected in the stratosphere, which implies a nonuniform temperature and aerosol distribution across the Jovian disk or across high- and low-pressure regions due to local atmospheric dynamics.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 86; Sept. 30
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  • 8
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    Observations of the 10-micron natural laser emission from the mesospheres of Mars and Venus (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Observations of the total flux and center to limb dependence of the nonthermal emission occurring in the cores of the 9.4 and 10.4 micrometers CO2 bands on Mars are compared to a theoretical model based on this mechanism. The model successfully reproduces the observed center to limb dependence of this emission, to within the limits imposed by the spatial resolution of the observations of Mars and Venus. The observed flux from Mars agrees closely with the prediction of the model; the flux observed from Venus is 74 percent of the flux predicted by the model. This emission is used to obtain the kinetic temperatures of the Martian and Venusian mesospheres. For Mars near 70 km altitude, a rotational temperature analysis using five lines gives T = 135 + or - 20 K. The frequency width of the emission is also analyzed to derive a temperature of 126 + or - 6 K. In the case of the Venusian mesosphere near 109 km, the frequency width of the emission gives T = 204 + or - 10 K.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 55; Sept
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  • 9
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    Measurements of stratospheric ethane in the Jovian South Polar Region from infrared heterodyne spectroscopy of the nu9 band near 12 microns (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Astrophysical Journal; vol. 265
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  • 10
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    The NASA/GISS Mars general circulation model: Preliminary experiments (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: The NASA/GISS Mars General Circulation Model (GCM) is an adapted version of the GISS Global Climate/Middle Atmosphere Model, specifically developed for the diagnostic validation and objective analysis of measured atmospheric temperatures from the Mars Observer Pressure Modulator Infrared Radiometer (PMIRR) experiment. The GISS Mars GCM has 23 vertical layers extending from the surface to approximately 80 km altitude, representing a vertical resolution of about 0.3 scale heights. The primitive (vertically hydrostatic) equations are solved in finite difference form on the Krakawa B grid, with a horizontal resolution of 8 deg x 10 deg (latitude-longitude). The model includes a diurnal solar cycle, heat transport within a two-layer ground, and a high-order 'slopes-scheme' for the advection of heat in the upper atmosphere. The radiative transfer scheme is based on the correlated k distribution method for the treatment of nongray gaseous absorption thermal emission, and multiple scattering, including options for suspended dust. A special feature of the model of particular importance for Mars is a parameterization of gravity-wave-induced drag incorporating orographic forcing, wind shear, convection, and radiative damping. The implementation of the GISS Mars model includes global maps of topography, roughness, and albedo.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Workshop on Atmospheric Transport on Mars; p 5
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