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  • PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR  (4)
  • Lunar and Planetary Exploration  (3)
  • Meteorology and Climatology  (2)
  • 1
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    The Galileo probe mass spectrometer: composition of Jupiter's atmosphere (1996)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: The composition of the jovian atmosphere from 0.5 to 21 bars along the descent trajectory was determined by a quadrupole mass spectrometer on the Galileo probe. The mixing ratio of He (helium) to H2 (hydrogen), 0.156, is close to the solar ratio. The abundances of methane, water, argon, neon, and hydrogen sulfide were measured; krypton and xenon were detected. As measured in the jovian atmosphere, the amount of carbon is 2.9 times the solar abundance relative to H2, the amount of sulfur is greater than the solar abundance, and the amount of oxygen is much less than the solar abundance. The neon abundance compared with that of hydrogen is about an order of magnitude less than the solar abundance. Isotopic ratios of carbon and the noble gases are consistent with solar values. The measured ratio of deuterium to hydrogen (D/H) of (5 +/- 2) x 10(-5) indicates that this ratio is greater in solar-system hydrogen than in local interstellar hydrogen, and the 3He/4He ratio of (1.1 +/- 0.2) x 10(-4) provides a new value for protosolar (solar nebula) helium isotopes. Together, the D/H and 3He/4He ratios are consistent with conversion in the sun of protosolar deuterium to present-day 3He.
    Keywords: Meteorology and Climatology
    Type: Science (ISSN 0036-8075); Volume 272; 5263; 846-9
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  • 2
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    Chemical composition measurements of the atmosphere of Jupiter with the Galileo Probe mass spectrometer (1998)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: The Galileo Probe entered the atmosphere of Jupiter on December 7, 1995. Measurements of the chemical and isotopic composition of the Jovian atmosphere were obtained by the mass spectrometer during the descent over the 0.5 to 21 bar pressure region over a time period of approximately 1 hour. The sampling was either of atmospheric gases directly introduced into the ion source of the mass spectrometer through capillary leaks or of gas, which had been chemically processed to enhance the sensitivity of the measurement to trace species or noble gases. The analysis of this data set continues to be refined based on supporting laboratory studies on an engineering unit. The mixing ratios of the major constituents of the atmosphere hydrogen and helium have been determined as well as mixing ratios or upper limits for several less abundant species including: methane, water, ammonia, ethane, ethylene, propane, hydrogen sulfide, neon, argon, krypton, and xenon. Analysis also suggests the presence of trace levels of other 3 and 4 carbon hydrocarbons, or carbon and nitrogen containing species, phosphine, hydrogen chloride, and of benzene. The data set also allows upper limits to be set for many species of interest which were not detected. Isotope ratios were measured for 3He/4He, D/H, 13C/12C, 20Ne/22Ne, 38Ar/36Ar and for isotopes of both Kr and Xe.
    Keywords: Meteorology and Climatology
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 21; 11; 1455-61
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  • 3
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    Asymptotic Relations Between the Thomas- Fermi-Dirac and Thomas-Fermi Atom Models. I (1967)
    In:  Other Sources
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    Publication Date: 2011-08-12
    Description: Asymptotic relations between Thomas-Fermi-Dirac and Thomas-Fermi atom models
    Keywords: PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR
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  • 4
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    Derivation of relations between temperature- perturbed Thomas-Fermi functions. (1966)
    In:  Other Sources
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    Publication Date: 2011-08-11
    Description: Temperature perturbation in Thomas-Fermi functions for atom radius as related by Gilvarry to simpler Feynman-Metropolis-Teller case
    Keywords: PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR
    Type: JOURNAL OF CHEMICAL PHYSICS
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  • 5
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    Asymptotic relations between the Thomas- Fermi-Dirac and Thomas-Fermi atom models. II - Extension of the case of low atomic number (1970)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Asymptotic relation between Thomas-Fermi-Dirac and Thomas-Fermi atom models for pressure with and without exchange, considering Coulomb contribution to energy
    Keywords: PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR
    Type: ; SEARCH(
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  • 6
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    Asymptotic relations between the Thomas- Fermi-Dirac and Thomas-Fermi atom models. 2. Extension of the case of low atomic number (1968)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Asymptotic relations between Thomas-Fermi-Dirac and Thomas-Fermi atomic models
    Keywords: PHYSICS, ATOMIC, MOLECULAR, AND NUCLEAR
    Type: NASA-TM-X-63284 , X-615-68-259
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  • 7
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    Initial PVO Evidence of Electron Depletion Signatures Downstream of Venus (1993)
    In:  CASI
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    Publication Date: 2019-08-17
    Description: This first analysis of Pioneer Venus Orbiter (PVO) plasma analyzer electron measurements obtained in early 1992 during the PVO entry phase of the mission indicates the presence downstream from the terminator of a depletion or "bite out" of energetic ionosheath electrons similar to that observed on Mariner 10. There is more than one possible explanation for this energetic electron depletion. If it is due to atmospheric scattering, the electrons traveling along draped magnetic flux tubes that thread through the Venus neutral atmosphere would lose energy from impact ionization with oxygen. The cross-section for such electron impact ionization of oxygen has a peak near 100 eV, and it remains high above this energy, so atmospheric loss could provide a natural process for electrons at these energies to be selectively removed. In this case, our results are consistent with the Kar et al. (1994) study of PVO atmospheric entry ion mass spectrometer data which indicates that electron impact plays a significant role in maintaining the nightside ionosphere. Although it is appealing to interpret the energetic electron depletion in terms of direct atmospheric scattering, alternatively it could result from strong draping which connects the depletion region magnetically to the weak downstream bow shock and thereby reduces the electron source strength.
    Keywords: Lunar and Planetary Exploration
    Type: Paper 93GL02483 , Geophysical Research Letters. Selected Papers on Pioneer Venus Orbiter: Entry Phase; 20; 23; 2779-2782; NASA-TM-112700
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  • 8
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    Ion Measurements During Pioneer Venus Reentry: Implications for Solar Cycle Variation of Ion Composition and Dynamics (1993)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: During the final, low solar activity phase of the Pioneer Venus mission, the Orbiter Ion Mass Spectrometer measurements found all ion species, in the midnight-dusk sector, reduced in concentration relative to that observed at solar maximum. Molecular ion species comprised a greater part of the total ion concentration as O(+) and H(+) had the greatest depletions. The nightside ionospheric states were strikingly similar to the isolated solar maximum "disappearing" ionospheres. Both are very dynamic states characterized by a rapidly drifting plasma and 30-100 eV superthermal O(+) ions.
    Keywords: Lunar and Planetary Exploration
    Type: Paper 93GL02239 , Geophysical Research Letters. Selected Papers on Pioneer Venus Orbiter: Entry Phase; 20; 23; 2735-2738; NASA-TM-112700
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  • 9
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    Plasma Escape from Unmagnetized Bodies (1998)
    In:  Other Sources
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    Publication Date: 2019-07-17
    Description: A considerable fraction of atmospheric loss at Venus and Titan is in the form of plasma escape. This is due in part to the fact that the ionospheres of these unmagnetized bodies interact directly with the high speed plasmas flowing around them. The similarities of the interactions help reinforce interpretations of measurements made at each body, especially when instruments and measurement sites differ. For example, it is well established through this method that ions born in the exospheres above the ionopauses are picked up and carried away by the solar wind at Venus and the rotating plasma in Saturn's magnetosphere. On the other hand, it is more difficult to relate the observations associated with escape of cooler ionospheric plasma down the ionotails of each body. A clear example of ionospheric plasma escaping Titan was observed as it flowed down its ionotail (1). Measurements at Venus have not as yet clearly distinguished between ionospheric and pickup ion escape in the ionotail; however, cold ions detected in the distant wake at 1 AU by the CELIAS/CTOF instrument on SOHO have been interpreted as ionospheric in origin (2). An algorithm to determine ionospheric flow from Pioneer Venus aeronomical measurements is used to show that escape of cold ionospheric plasma is likely to occur. These results along with plasma flow measurements made in the ionotail of Venus are combined and compared to the corresponding flow at Titan.
    Keywords: Lunar and Planetary Exploration
    Type: Dec 06, 1998 - Dec 10, 1998; San Francisco, CA; United States
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