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  • 1
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    Galileo ultraviolet spectrometer experiment: initial venus and interplanetary cruise results (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-09-27
    Description: The Galileo Extreme Ultraviolet Spectrometer obtained a spectrum of Venus atmospheric emissions in the 55.0- to 125.0-nanometer (nm) wavelength region. Emissions of helium (58.4 nm), ionized atomic oxygen (83.4 nm), and atomic hydrogen (121.6 nm), as well as a blended spectral feature of atomic hydrogen (Lyman-beta) and atomic oxygen (102.5 nm), were observed at 3.5-nm resolution. During the Galileo spacecraft cruise from Venus to Earth, Lyman-alpha emission from solar system atomic hydrogen (121.6 nm) was measured. The dominant source of the Lyman-alpha emission is atomic hydrogen from the interstellar medium. A model of Galileo observations at solar maximum indicates a decrease in the solar Lyman-alpha flux near the solar poles. A strong day-to-day variation also occurs with the 27-day periodicity of the rotation of the sun.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hord, C W -- Barth, C A -- Esposito, L W -- McClintock, W E -- Pryor, W R -- Simmons, K E -- Stewart, A I -- Thomas, G E -- Ajello, J M -- Lane, A L -- West, R W -- Sandel, B R -- Broadfoot, A L -- Hunten, D M -- Shemansky, D E -- New York, N.Y. -- Science. 1991 Sep 27;253(5027):1548-50.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17784100" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 2
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    Ultraviolet spectrometer observations of neptune and triton (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-12-15
    Description: Results from the occultation of the sun by Neptune imply a temperature of 750 +/- 150 kelvins in the upper levels of the atmosphere (composed mostly of atomic and molecular hydrogen) and define the distributions of methane, acetylene, and ethane at lower levels. The ultraviolet spectrum of the sunlit atmosphere of Neptune resembles the spectra of the Jupiter, Saturn, and Uranus atmospheres in that it is dominated by the emissions of H Lyman alpha (340 +/- 20 rayleighs) and molecular hydrogen. The extreme ultraviolet emissions in the range from 800 to 1100 angstroms at the four planets visited by Voyager scale approximately as the inverse square of their heliocentric distances. Weak auroral emissions have been tentatively identified on the night side of Neptune. Airglow and occultation observations of Triton's atmosphere show that it is composed mainly of molecular nitrogen, with a trace of methane near the surface. The temperature of Triton's upper atmosphere is 95 +/- 5 kelvins, and the surface pressure is roughly 14 microbars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Broadfoot, A L -- Atreya, S K -- Bertaux, J L -- Blamont, J E -- Dessler, A J -- Donahue, T M -- Forrester, W T -- Hall, D T -- Herbert, F -- Holberg, J B -- Hunter, D M -- Krasnopolsky, V A -- Linick, S -- Lunine, J I -- McConnell, J C -- Moos, H W -- Sandel, B R -- Schneider, N M -- Shemansky, D E -- Smith, G R -- Strobel, D F -- Yelle, R V -- New York, N.Y. -- Science. 1989 Dec 15;246(4936):1459-66.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17756000" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 3
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    Extreme ultraviolet observations from voyager 1 encounter with jupiter (1979)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1979-06-01
    Description: Observations of the optical extreme ultraviolet spectrum of the Jupiter planetary system during the Voyager 1 encounter have revealed previously undetected physical processes of significant proportions. Bright emission lines of S III, S IV, and O III indicating an electron temperature of 10(5) K have been identified in preliminary analyses of the Io plasma torus spectrum. Strong auroral atomic and molecular hydrogen emissions have been observed in the polar regions of Jupiter near magnetic field lines that map the torus into the atmosphere of Jupiter. The observed resonance scattering of solar hydrogen Lyman alpha by the atmosphere of Jupiter and the solar occultation experiment suggest a hot thermosphere (〉/= 1000 K) wvith a large atomic hydrogen abundance. A stellar occultation by Ganymede indicates that its atmosphere is at most an exosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Broadfoot, A L -- Belton, M J -- Takacs, P Z -- Sandel, B R -- Shemansky, D E -- Holberg, J B -- Ajello, J M -- Atreya, S K -- Donahue, T M -- Moos, H W -- Bertaux, J L -- Blamont, J E -- Strobel, D F -- McConnell, J C -- Dalgarno, A -- Goody, R -- McElroy, M B -- New York, N.Y. -- Science. 1979 Jun 1;204(4396):979-82.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17800434" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
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    Extreme ultraviolet observations from voyager 1 encounter with saturn (1981)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1981-04-10
    Description: The global hydrogen Lyman alpha, helium (584 angstroms), and molecular hydrogen band emissions from Saturn are qualitatively similar to those of Jupiter, but the Saturn observations emphasize that the H(2) band excitation mechanism is closely related to the solar flux. Auroras occur near 80 degrees latitude, suggesting Earth-like magnetotail activity, quite different from the dominant Io plasma torus mechanism at Jupiter. No ion emissions have been detected from the magnetosphere of Saturn, but the rings have a hydrogen atmosphere; atomic hydrogen is also present in a torus between 8 and 25 Saturn radii. Nitrogen emission excited by particles has been detected in the Titan dayglow and bright limb scans. Enhancement of the nitrogen emission is observed in the region of interaction between Titan's atmosphere and the corotating plasma in Saturn's plasmasphere. No particle-excited emission has been detected from the dark atmosphere of Titan. The absorption profile of the atmosphere determined by the solar occultation experiment, combined with constraints from the dayglow observations and temperature information, indicate that N(2) is the dominant species. A double layer structure has been detected above Titan's limb. One of the layers may be related to visible layers in the images of Titan.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Broadfoot, A L -- Sandel, B R -- Shemansky, D E -- Holberg, J B -- Smith, G R -- Strobel, D F -- McConnell, J C -- Kumar, S -- Hunten, D M -- Atreya, S K -- Donahue, T M -- Moos, H W -- Bertaux, J L -- Blamont, J E -- Pomphrey, R B -- Linick, S -- New York, N.Y. -- Science. 1981 Apr 10;212(4491):206-11.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17783831" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 5
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    Extreme ultraviolet observations from the voyager 2 encounter with saturn (1982)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1982-01-29
    Description: Combined analysis of helium (584 angstroms) airglow and the atmospheric occultations of the star delta Scorpii imply a vertical mixing parameter in Saturn's upper atmosphere of K (eddy diffusion coefficient) approximately 8 x 10(7) square centimeters per second, an order of magnitude more vigorous than mixing in Jupiter's upper atmosphere. Atmospheric H(2) band absorption of starlight yields a preliminary temperature of 400 K in the exosphere and a temperature near the homopause of approximately 200 K. The energy source for the mid-latitude H(2) band emission still remains a puzzle. Certain auroral emissions can be fully explained in terms of electron impact on H(2), and auroral morphology suggests a link between the aurora and the Saturn kilometric radiation. Absolute optical depths have been determined for the entire C ring andparts of the A and B rings. A new eccentric ringlet has been detected in the C ring. The extreme ultraviolet reflectance of the rings is fairly uniform at 3.5 to 5 percent. Collisions may control the distribution of H in Titan's H torus, which has a total vertical extent of approximately 14 Saturn radii normal to the orbit plane.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sandel, B R -- Shemansky, D E -- Broadfoot, A L -- Holberg, J B -- Smith, G R -- McConnell, J C -- Strobel, D F -- Atreya, S K -- Donahue, T M -- Moos, H W -- Hunten, D M -- Pomphrey, R B -- Linick, S -- New York, N.Y. -- Science. 1982 Jan 29;215(4532):548-53.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17771276" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 6
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    Extreme ultraviolet observations from voyager 2 encounter with jupiter (1979)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1979-11-23
    Description: Extreme ultraviolet spectral observations of the Jovian planetary system made during the Voyager 2 encounter have extended our knowledge of many of the phenomena and physical processes discovered by the Voyager 1 ultraviolet spectrometer. In the 4 months between encounters, the radiation from Io's plasma torus has increased in intensity by a factor of about 2. This change was accompanied by a decrease in plasma temperature of about 30 percent. The high-latitude auroral zones have been positively associated with the magnetic projection of the plasma torus onto the planet. Emission in molecular hydrogen bands has been detected from the equatorial regions of Jupiter, indicating planetwide electron precipitation. Hydrogen Lyman alpha from the dark side of the planet has been measured at an intensity of about 1 kilorayleigh. An observation of the occultation of alpha Leonis by Jupiter was carried out successfully and the data are being analyzed in detail.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sandel, B R -- Shemansky, D E -- Broadfoot, A L -- Bertaux, J L -- Blamont, J E -- Belton, M J -- Ajello, J M -- Holberg, J B -- Atreya, S K -- Donahue, T M -- Moos, H W -- Strobel, D F -- McConnell, J C -- Dalgarno, A -- Goody, R -- McElroy, M B -- Takacs, P Z -- New York, N.Y. -- Science. 1979 Nov 23;206(4421):962-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17733915" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 7
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    Ultraviolet spectrometer observations of uranus (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1986-07-04
    Description: Data from solar and stellar occultations of Uranus indicate a temperature of about 750 kelvins in the upper levels of the atmosphere (composed mostly of atomic and molecular hydrogen) and define the distributions of methane and acetylene in the lower levels. The ultraviolet spectrum of the sunlit hemisphere is dominated by emissions from atomic and molecular hydrogen, which are kmown as electroglow emissions. The energy source for these emissions is unknown, but the spectrum implies excitation by low-energy electrons (modeled with a 3-electron-volt Maxwellian energy distribution). The major energy sink for the electrons is dissociation of molecular hydrogen, producing hydrogen atoms at a rate of 10(29) per second. Approximately half the atoms have energies higher than the escape energy. The high temperature of the atmosphere, the small size of Uranus, and the number density of hydrogen atoms in the thermosphere imply an extensive thermal hydrogen corona that reduces the orbital lifetime of ring particles and biases the size distribution toward larger particles. This corona is augmented by the nonthermal hydrogen atoms associated with the electroglow. An aurora near the magnetic pole in the dark hemisphere arises from excitation of molecular hydrogen at the level where its vertical column abundance is about 10(20) per square centimeter with input power comparable to that of the sunlit electroglow (approximately 2x10(11) watts). An initial estimate of the acetylene volume mixing ratio, as judged from measurements of the far ultraviolet albedo, is about 2 x 10(-7) at a vertical column abundance of molecular hydrogen of 10(23) per square centimeter (pressure, approximately 0.3 millibar). Carbon emissions from the Uranian atmosphere were also detected.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Broadfoot, A L -- Herbert, F -- Holberg, J B -- Hunten, D M -- Kumar, S -- Sandel, B R -- Shemansky, D E -- Smith, G R -- Yelle, R V -- Strobel, D F -- Moos, H W -- Donahue, T M -- Atreya, S K -- Bertaux, J L -- Blamont, J E -- McConnell, J C -- Dessler, A J -- Linick, S -- Springer, R -- New York, N.Y. -- Science. 1986 Jul 4;233(4759):74-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17812892" target="_blank"〉PubMed〈/a〉
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  • 8
    Electronic Resource
    Electronic Resource
    Morphology of Saturn's aurora (1981)
    [s.l.] : Nature Publishing Group
    Nature 292 (1981), S. 679-682 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] BECAUSE Saturn possesses a dense atmosphere and a strong magnetic field, it is reasonable to expect that aurorae should also be present. Before the encounter of Voyager 1, two lines of evidence suggested the presence of polar aurora on Saturn, but both admitted alternate interpretations. Pioneer ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/292679a0
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  • 9
    Electronic Resource
    Electronic Resource
    Galileo Ultraviolet Spectrometer experiment (1992)
    Springer
    Space science reviews 60 (1992), S. 503-530 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract 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 × 0.1 deg for illuminated disc observations and 1 deg × 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 × 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.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00216866
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  • 10
    Electronic Resource
    Electronic Resource
    Ultraviolet spectrometer experiment for the Voyager mission (1977)
    Springer
    Space science reviews 21 (1977), S. 183-205 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Voyager Ultraviolet Spectrometer (UVS) is an objective grating spectrometer covering the wavelength range of 500–1700 Å with 10 Å resolution. Its primary goal is the determination of the composition and structure of the atmospheres of Jupiter, Saturn, Uranus and several of their satellites. The capability for two very different observational modes have been combined in a single instrument. Observations in the airglow mode measure radiation from the atmosphere due to resonant scattering of the solar flux or energetic particle bombardment, and the occultation mode provides measurements of the atmospheric extinction of solar or stellar radiation as the spacecraft enters the shadow zone behind the target. In addition to the primary goal of the solar system atmospheric measurements, the UVS is expected to make valuable contributions to stellar astronomy at wavelengths below 1000 Å.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00200850
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