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  • 1
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    Galileo Ultraviolet Spectrometer experiment (1992)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: The Galileo ultraviolet spectrometer experiment uses data obtained by the Ultraviolet Spectrometer (UVS) mounted on the pointed orbiter scan platform and from the Extreme Ultraviolet Spectrometer (EUVS) mounted on the spinning part of the orbiter with the field of view perpendicular to the spin axis. The UVS is a Ebert-Fastie design that covers the range 113-432 nm with a wavelength resolution of 0.7 nm below 190 and 1.3 nm at longer wavelengths. The UVS spatial resolution is 0.4 deg x 0.1 deg for illuminated disk observations and 1 deg x 0.1 deg for limb geometries. The EUVS is a Voyager design objective grating spectrometer, modified to cover the wavelength range from 54 to 128 nm with wavelength resolution 3.5 nm for extended sources and 1.5 nm for point sources and spatial resolution of 0.87 deg x 0.17 deg. The EUVS instrument will follow up on the many Voyager UVS discoveries, particularly the sulfur and oxygen ion emissions in the Io torus and molecular and atomic hydrogen auroral and airglow emissions from Jupiter. The UVS will obtain spectra of emission, absorption, and scattering features in the unexplored, by spacecraft, 170-432 nm wavelength region. The UVS and EUVS instruments will provide a powerful instrument complement to investigate volatile escape and surface composition of the Galilean satellites, the Io plasma torus, micro- and macro-properties of the Jupiter clouds, and the composition structure and evolution of the Jupiter upper atmosphere.
    Keywords: SPACECRAFT INSTRUMENTATION
    Type: Space Science Reviews (ISSN 0038-6308); 60; 1-4,
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  • 2
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    Electron impact excitation and dissociation of N2 via the b 1Pi(u) state (1991)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Electron impact excitation of the b 1Pi(u) state in N2 plays a prominent role in the dissociation of the molecule and thus in the production of atomic nitrogen in planetary atmospheres. Electron impact excitation cross sections combined with electron-impact-induced fluorescence measurements can yield the corresponding dissociation cross sections. Serious discrepancies exist among excitation cross sections reported in the literature. To clarify the situation, these cross sections were measured at two impact energies using electron energy loss spectroscopy. The new results are in agreement with recent values deduced from optical measurements and fall midway between previous results which are too high or low by factors of 2.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 96; 17
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  • 3
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    Electron impact excitation cross section studies of methane and acetylene (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The 40-200-nm emission features of electron-impact-excited CH4 and C2H2 are investigated experimentally using the crossed-beam apparatus and VUV calibration techniques described by Ajello et al. (1982 and 1985). The results are presented in extensive tables and graphs and characterized in detail. All of the features are attributed to the atomic dissociation fragments C I, C II, and H, and the long lifetimes and high kinetic energies of the excited H fragments are shown to truncate the H Lyman series near principal quantum number n = 10.
    Keywords: ATOMIC AND MOLECULAR PHYSICS
    Type: Journal of Chemical Physics (ISSN 0021-9606); 86; 2750-276
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  • 4
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    No cometesimals in the inner solar system (1988)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Ultraviolet measurements made by Voyager 2, apparently showing a rapid decrease in hydrogen Lyman-alpha emission with distance from the sun, were taken by Donahue et al. (1987) as evidence for a source of atomic hydrogen in the very local interstellar medium (VLISM). The suggested source of the hydrogen is a class of small comets at solar distances of about 1 AU. This claim has been adduced as evidence for a theory that the earth is subject to a large influx of cometary material significantly affecting atmospheric evolution. The Voyager 2 data have been reanalyzed, and it is shown that no source of hydrogen in the VLISM is required other than the inflow of neutral atoms.
    Keywords: ASTROPHYSICS
    Type: Nature (ISSN 0028-0836); 335; 417-419
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  • 5
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    A reexamination of important N2 cross sections by electron impact with application to the dayglow - The Lyman-Birge-Hopfield band system and N I (1199.99 nm) (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: The emission cross section (cascade plus direct excitation) and predissociation cross section for the Lyman-Birge-Hopfield band systems is experimentally measured. The results are compared to electron energy loss measurements of the direct excitation cross section. An analytic approximation to the measured cross section is obtained which demonstrates the extreme simplicity of the collision strengths at energies above the cross-section peak. Cross sections are also obtained for the FUV atomic nitrogen multiplets. Available cross sections for N I emission at 119.99 nm are discussed in detail.
    Keywords: GEOPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 9845-986
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  • 6
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    (abstract)Electron Impact Emission Cross Sections for Modeling UV Auroral and Dayglow Observations of the Upper Atmospheres of Planets (1993)
    In:  Other Sources
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    Publication Date: 2018-06-08
    Description: In the upper atmospheres of the Jovian and Terrestrial planets a dominant mechanism for energy transfer occurs through electron collisional processes with neutral species leading to UV radiation. In response to the need for accurate collision cross sections to model spectroscopic observations of planetary systems, JPL has measured in the laboratory emission cross sections and medium resolution spectra of H, H(sub 2), N(sub 2), SO(sub 2), and other important planetary gases.Voyager and International Ultraviolet Explorer (IUE) spacecraft have established that band systems of H(sub 2) and N(sub 2) are the dominant UV molecular emissions in the solar system produced by electron impact. Applications of our data to models of Voyager, IUE, Galileo, and Hubble Space Telescope observations of the planets will be described.
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  • 7
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    The Electron Excitation Function of H Lyman-(alpha) from Threshold to 1.8 keV (1996)
    In:  Other Sources
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    Publication Date: 2018-06-08
    Description: The excitation function of prompt Lyman-(alpha) radiation, produced by electron impact excitation of atomic hydrogen, has been measured for the first time over an extended energy range from threshold to 1.8 keV. Measurments were obtained in a crossed-beams experiment using both magnetically confined and electrostatically focused electrons in collision with atomic hydrogen produced by an intense discharge source.
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  • 8
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    Hydrogen emission from Jupiter: Hydrogen emission from sunlit atmosphere of Saturn (1987)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Successful IUE observations of the equatorial sunlit atmosphere of Jupiter and Saturn have been obtained. Spectra containing atomic and molecular hydrogen and solar reflection continuum emissions have been analyzed, with the purpose of determining the long term temporal behavior of the electroglow process. Quantitative estimates have been established for the first time using a model analysis of the short wavelength region of the spectrum. Both systems show varying degrees of long term variability in hydrogen emission rate, but the time scale is too short to determine whether there is a dependence on solar cycle activity. As part of the emission modeling program, a preliminary point source spreading function for the IUE SWP instrument has been established, suggesting a wavelength dependence in spectral line width different from previous analyses. Further IUE observations are planned for both Jupiter and Saturn.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-180245 , NAS 1.26:180245
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  • 9
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    The Saturn System as Observed by Cassini's Ultraviolet Imaging Spectrograph (2005)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: The Cassini Ultraviolet Imaging Spectrograph (UVIS) has major new findings in all aspects of Saturn science: Saturn, its rings, Titan and the icy satellites, and the Saturn magnetosphere. Dynamic interactions between neutrals, ions, rings, moons and meteoroids produce a highly structured and time variable Saturn system. Highlights and outstanding new results will be reported, focusing on Saturn s moons and their interaction with their environment. The UVIS is one of Cassini s suite of remote sensing instruments. The UVIS instrument includes channels for extreme UV (55 to 110 nm) and far UV (110 to 190 nm) spectroscopic imaging, high speed photometry of stellar occultations, solar EUV occultation, and a hydrogen/deuterium absorption cell. UVIS has detected products of water dissociation, neutral oxygen and OH, which dominate the Saturn inner magnetosphere, in contrast to Jupiter, and H fills the entire magnetosphere apparently extending through the magnetopause at far greater density than the ion population. The O and OH and a fraction of the H are probably the products of water physical chemistry, and derived ultimately from water ice. Observed fluctuations indicate close interactions with plasma sources. Sputtering from the satellites water ice surfaces is insufficient to supply the observed mass. Stochastic events in the E ring may be the ultimate source.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 5; LPI-Contrib-1234-Pt-5
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  • 10
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    A reanalysis of Voyager UVS observations of Titan (1992)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Data from the Voyager 1 Ultraviolet Spectrometer (UVS) encounter at Titan were reanalyzed to reveal new spatial and spectral information. The observations, data reduction and spectrum analysis are discussed. The following conclusions were drawn: Titan's airglow is driven by a combination of mechanisms including both EUV deposition and magnetospheric particle precipitation; the emissions are distributed throughout a range of altitudes in the atmosphere; enhanced nightside emissions of the Helium 58.4 nm line may be the result of a thermospheric diurnal temperature variation; the CD2 spectrum, with enhanced Ly(alpha) and N-2 64.5 and 67.0 nm emission, implies that some of the high altitude excitation is due to impact dissociative excitation of N2 by electrons with E greater than 150 eV; the CD2 spectrum is consistent with the existence of a high altitude bright spot in the dayside disk with dimensions from 400 to 900 km.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: ESA, Symposium on Titan; p 67-74
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