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  • 1
    Electronic Resource
    Electronic Resource
    Origin of the major planet atmospheres: Clues from trace species (1994)
    Springer
    Earth, moon and planets 67 (1994), S. 71-75 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00613292
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    Paper (German National Licenses)
    Fulltext
  • 2
    Electronic Resource
    Electronic Resource
    Galileo Probe Mass Spectrometer experiment (1992)
    Springer
    Space science reviews 60 (1992), S. 111-142 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Galileo Probe Mass Spectrometer (GPMS) is a Probe instrument designed to measure the chemical and isotopic composition including vertical variations of the constituents in the atmosphere of Jupiter. The measurement will be performed by in situ sampling of the ambient atmosphere in the pressure range from approximately 150 mbar to 20 bar. In addition batch sampling will be performed for noble gas composition measurement and isotopic ratio determination and for sensitivity enhancement of non-reactive trace gases. The instrument consists of a gas sampling system which is connected to a quadrupole mass analyzer for molecular weight analysis. In addition two sample enrichment cells and one noble gas analysis cell are part of the sampling system. The mass range of the quadrupole analyzer is from 2 amu to 150 amu. The maximum dynamic range is 108. The detector threshold ranges from 10 ppmv for H2O to 1 ppbv for Kr and Xe. It is dependent on instrument background and ambient gas composition because of spectral interference. The threshold values are lowered through sample enrichment by a factor of 100 to 500 for stable hydrocarbons and by a factor of 10 for noble gases. The gas sampling system and the mass analyzer are sealed and evacuated until the measurement sequence is initiated after the Probe enters into the atmosphere of Jupiter. The instrument weighs 13.2 kg and the average power consumption is 13 W. The instrument follows a sampling sequence of 8192 steps and a sampling rate of two steps per second. The measurement period lasts appropriately 60 min through the nominal pressure and altitude range.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00216852
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    Paper (German National Licenses)
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  • 3
    Electronic Resource
    Electronic Resource
    The use of a water-soluble formazan complex to quantitate the cell number and mitochondrial function ofLeishmania major promastigotes (1994)
    Springer
    Parasitology research 80 (1994), S. 235-239 
    Details
    ISSN: 1432-1955
    Source: Springer Online Journal Archives 1860-2000
    Topics: Biology , Medicine
    Notes: Abstract One of the methods to quantitateLeishmania major promastigotes (LmP) has been to utilize the formation of a formazan dye, which in turn is produced via conversion of an artificial substrate, 3-(4,5-dimethylthiazol-2-yl)-2,5-diphenyltetrazolium bromide (MTT). The method has one major drawback in that the formazan complex precipitates inside the parasites and has to be extracted by denaturants before measurements can be performed. By using a new synthetic substrate, 3-(4,5-dimethylthiazol-2-yl)-5-(3-carboxymethoxyphenyl)-2-(4-sulfonyl)-2H-tetrazolium (MTS), the extraction procedure is eliminated as the formazan-like dye is released spontaneously into the medium, making it possible to perform several measurements on the same parasite culture without disturbing or killing the parasites. The measurements were shown to reflect the numbers of parasites as confirmed via comparative experiments using radioactive thymidine uptake and cell counting, respectively. The method is simple, fast, and highly reproducible and is suitable for drug screening, identification of drug-resistant isolates, and growth-kinetics studies. It is therefore contemplated that the MTS method will be a general and useful technique in this field of parasitology.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00932680
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  • 4
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    Origin of the major planet atmospheres: Clues from trace species (1994)
    Springer
    Details
    Publication Date: 1994-01-01
    Print ISSN: 0167-9295
    Electronic ISSN: 1573-0794
    Topics: Geosciences , Physics
    Published by Springer
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    PAPER CURRENT
  • 5
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    Constraints on N2 in Neptune's atmosphere from Voyager measurements (1993)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: It is shown that N2 may be present in the troposphere of Neptune in an amount difficult to evaluate but which could easily be as high as 0.003, while there is no evidence that it is present in the atmosphere of Uranus. The estimate of the helium abundance depends on the assumed value for N2. If there is no N2 in the observed region of the atmosphere of Uranus and an N2 mole fraction of 0.003 on Neptune, the central value of the estimates of the helium abundance are equal to 0.26 by mass in both planets, which is close to the protosolar value of 0.28. This would imply that the He/H2 ratios measured in the outer atmospheres of Uranus and Neptune are representative of the ratio in the primitive solar nebula and thus were not modified during planetary formation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 101; 1; p. 168-171.
    Format: text
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    NASA TECHNICAL REPORTS
  • 6
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    Galileo Probe Mass Spectrometer experiment (1992)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: The chemical and isotopic composition of the Jupiter atmosphere's constituents, including their vertical variations, will be measured by the Galileo Probe Mass Spectrometer instrument through in situ sampling; batch sampling will also be undertaken for noble gas composition and isotopic ratio determinations. The instrument's gas-sampling system is connected to a quadrupole mass analyzer for molecular weight analysis. Threshold values are lowered through sample enrichment by a factor of 100-500 for stable hydrocarbons and by a factor of 10 for noble gases. The instrument follows a sampling sequence of 8192 steps, at a rate of 2 steps/sec.
    Keywords: SPACECRAFT INSTRUMENTATION
    Type: Space Science Reviews (ISSN 0038-6308); 60; 1-4,
    Format: text
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    NASA TECHNICAL REPORTS
  • 7
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    The temperature of nitrogen on Pluto (1994)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: With Hapke scattering theory and absorption coefficients derived from our laboratory measurements of solid N2 we have modeled the spectrum of Triton. By comparing a Hapke scattering model to the measured spectrum from Triton, we determined the temperature of the N2 on the satellite's surface to be 38 (+2, -1) K which is in accord with the measurements of Voyager 2. Applying this technique to Pluto we find that the temperature of N2 on that body is 40 +/- 2 K. Other aspects of this investigation are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., The Twenty-Fifth Lunar and Planetary Science Conference. Part 3: P-Z; p 1419-1420
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 8
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    Determination of the Temperature of Nitrogen on Pluto from Spectral Measurements (1993)
    In:  Other Sources
    Details
    Publication Date: 2018-06-08
    Keywords: Lunar and Planetary Science and Exploration
    Format: text
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    NASA TECHNICAL REPORTS
  • 9
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    Detection of the 3.4- and 2.8-micron emission features in Comet Bradfield (1987s) (1990)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Comet Bradfield's 3.4-micron C-H emission feature at 3.4 microns, as well as the emission feature near 2.8 microns, exhibit spectral shapes similar to those noted in Comets Halley and Wilson; the derived abundances of the C-H bonds in all three comets are also comparable (within water production rate uncertainties). These data support the hypothesis that the species responsible for the 3.4- and 2.8-micron features may be common to all comets. Beyond this, the widely differing ages of the three comets suggest that the 3.4-micron feature-emitting organics are not the product of surface irradiation processes after the comets' formation.
    Keywords: ASTROPHYSICS
    Type: Icarus (ISSN 0019-1035); 83; 434-440
    Format: text
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    NASA TECHNICAL REPORTS
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