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  • 1
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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〉
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  • 2
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    The Galileo probe mass spectrometer: composition of Jupiter's atmosphere (1996)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1996-05-10
    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.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Niemann, H B -- Atreya, S K -- Carignan, G R -- Donahue, T M -- Haberman, J A -- Harpold, D N -- Hartle, R E -- Hunten, D M -- Kasprzak, W T -- Mahaffy, P R -- Owen, T C -- Spencer, N W -- Way, S H -- New York, N.Y. -- Science. 1996 May 10;272(5263):846-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Goddard Space Flight Center, Greenbelt, MD 20771, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/8629016" target="_blank"〉PubMed〈/a〉
    Keywords: Ammonia/analysis ; *Atmosphere ; Carbon/analysis ; *Extraterrestrial Environment ; Helium/analysis ; Hydrogen/analysis ; *Jupiter ; Mass Spectrometry ; Nitrogen/analysis ; Noble Gases/analysis ; Oxygen/analysis ; Water/*analysis
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  • 3
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    Evolution of a nitrogen atmosphere on titan (1978)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1978-08-18
    Description: Photochemical calculations indicate that if NH(3) outgassed from Titan it should have been converted to a dense N(2) atmosphere during the lifetime of the satellite. A crucial step in the process involves a gas phase reaction of N(2)H(4) with H. The most favorable conditions for this step would be the intermediate production of a CH(4)-H(2) greenhouse capable of raising the gas temperature to 150 degrees K. Subsequently about 20 bars of N(2) could have evolved. The pressure-induced opacity of 20 bars of N(2) should suffice to explain the recently measured 200 degrees K surface temperature. Unlike the situation on Jupiter, NH(3) is not recycled on Titan by reactions involving N(2) or N(2)H(4). This may explain the failure of recent attempts to detect NH(3) in the upper atmosphere of Titan.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Atreya, S K -- Donahue, T M -- Kuhn, W R -- New York, N.Y. -- Science. 1978 Aug 18;201(4356):611-3.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17794121" target="_blank"〉PubMed〈/a〉
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  • 4
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    Extreme ultraviolet observations from voyager 1 encounter with jupiter (1979)
    American Association for the Advancement of Science (AAAS)
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    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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  • 5
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    Pioneer venus results: an overview (1979)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1979-07-06
    Description: A summary is presented of the scientific results obtained during the first 120 days of the Pioneer Venus orbiter mission and produced by analysis of multiprobe data as of about 1 April 1979. The summary is essentially a guide to the material presented in the reports devoted to Pioneer Venus results in this issue of Science.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Donahue, T M -- New York, N.Y. -- Science. 1979 Jul 6;205(4401):41-4.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17778895" target="_blank"〉PubMed〈/a〉
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  • 6
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    Venus lower atmospheric composition: preliminary results from pioneer venus (1979)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1979-02-23
    Description: Initial examination of data from the neutral mass spectrometer on the Pioneer Venus sounder probe indicates that the abundances of argon-36, argon-38, and neon-20 in the Venus atmosphere are much higher than those of the corresponding gases in Earth's atmosphere, although the abundance of radiogenic argon-40 is apparently similar for both planets. The lower atmosphere of Venus includes significant concentrations of various gaseous sulfur compounds. The inlet leak to the mass spectrometer was temporarily blocked by an apparently liquid component of the Venus clouds during passage through the dense cloud layer. Analysis of gases released during the evaporation of the droplets shows the presence of water vapor to some compound or compounds of sulfur.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hoffman, J H -- Hodges, R R Jr -- McElroy, M B -- Donahue, T M -- Kolpin, M -- New York, N.Y. -- Science. 1979 Feb 23;203(4382):800-2.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17833003" target="_blank"〉PubMed〈/a〉
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  • 7
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    Composition and structure of the venus atmosphere: results from pioneer venus (1979)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1979-07-06
    Description: Results from the Pioneer Venus sounder probe neutral mass spectrometer indicate that there is no difference in the isotopic ratios of carbon and oxygen between Venus and Earth to within +/- 5 percent. The mixing ratio of nitrogen is 3.5(+3)(-2) percent with an isotopic ratio within 20 percent of that of Earth. The ratio of argon-36 to argon-40 is 85 percent, and the ratio of argon-38 to argon-36 is 20 percent. The mixing ratios of argon-36 and argon-40 are approximately 40 and 50 parts per million, respectively, with an error of about a factor of 2 (mainly toward a lesser amount) resulting from uncertainty in the response of the ion pump to rare gases. Hydrogen chloride cannot account for more than a few percent of the 36 mass peak, and therefore the large excess of primordial argon is a reasonable conclusion. The ratio of neon-20 to argon-36 of 0.5 +/- 0.3 is definitely terrestrial in character rather than solar. These results indicate that there is a large excess of all primordial noble gases on Venus relative to Earth. There appears to be a considerably higher abundance of sulfur compounds below 20 kilometers than in or above the main cloud layer. The 32 and 60 mass peaks show a sharp increase below 22 kilometers, indicating the possible production of sulfur and carbon oxysulfide (COS) at the expense of sulfur dioxide.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hoffman, J H -- Hodges, R R Jr -- McElroy, M B -- Donahue, T M -- Kolpin, M -- New York, N.Y. -- Science. 1979 Jul 6;205(4401):49-52.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17778898" target="_blank"〉PubMed〈/a〉
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  • 8
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    Ionosphere of venus: first observations of day-night variations of the ion composition (1979)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1979-07-06
    Description: The Bennett radio-frequency ion mass spectrometer on the Pioneer Venus orbiter is returning the first direct composition evidence of the processes responsible for the formation and maintenance of the nightside ionosphere. Early results from predusk through the nightside in the solar zenith angle range 63 degrees (dusk) to 120 degrees (dawn) reveal that, as on the dayside, the lower nightside ionosphere consists of F(1)and F(2) layers dominated by O(2)(+) and O(+), respectively. Also like the dayside, the nightside composition includes distributions of NO(+), C(+), N(+), H(+), He(+), CO(2)(+), and 28(+) (a combination of CO(+) and N(2)(+)). The surprising abundance of the nightside ionosphere appears to be maintained by the transport of O(+) from the dayside, leading also to the formation of O(2)(+) through charge exchange with CO(2). Above the exobase, the upper nightside ionosphere exhibits dramatic variability in apparent response to variations in the solar wind and interplanetary magnetic field, with the ionopause extending to several thousand kilometers on one orbit, followed by the complete rertnoval of thermal ions to altitudes below 200 kilometers on the succeeding orbit, 24 hours later. In the upper ionosphere, considerable structure is evident in many of the nightside ion profiles. Also evident are horizontal ion drifts with velocities up to the order of 1 kilometer per second. Whereas the duskside ionopause is dominated by O(+) H(+) dominates the topside on the dawnside of the antisolar point, indicating two separate regions for ion depletion in the magnetic tail regions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Taylor, H A Jr -- Brinton, H C -- Bauer, S J -- Hartle, R E -- Cloutier, P A -- Daniell, R E Jr -- Donahue, T M -- New York, N.Y. -- Science. 1979 Jul 6;205(4401):96-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17778915" target="_blank"〉PubMed〈/a〉
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  • 9
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    Ionosphere of venus: first observations of the dayside ion composition near dawn and dusk (1979)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1979-02-23
    Description: The first in situ measurements of the composition of the ionosphere of Venus are provided by independent Bennett radio-frequency ion mass spectrometers on the Pioneer Venus bits and orbiter spacecraft, exploring the dawn and duskside regions, respectively. An extensive composition of ion species, rich in oxygen, nitrogen, and carbon chemistry is idenitified. The dominant topside ion is O(+), with C(+), N(+), H(+), and He(+) as prominent secondary ions. In the lower ionosphere, the ionzization peak or F(1) layer near 150 kilometers reaches a concentration of about 5 x l0(3) ions per cubic centimeter, and is composed of the dominant molecular ion, O(2)(+), with NO(+), CO(+), and CO(2)(+), constituting less than 10 percent of the total. Below the O(+) peak near 200 kilometers, the ions exhibit scale heights consistent with a neutral gas temperature of about 180 K near the terminator. In the upper ionosphere, scale heights of all species reflect the effects of plasma transport, which lifts the composition upward to the often abrupt ionopause, or thermal ion boundary, which is observed to vary in height between 250 to 1800 kilometers, in response to solar wind dynamics.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Taylor, H A Jr -- Brinton, H C -- Bauer, S J -- Hartle, R E -- Donahue, T M -- Cloutier, P A -- Michel, F C -- Daniell, R E Jr -- Blackwell, B H -- New York, N.Y. -- Science. 1979 Feb 23;203(4382):752-4.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17832985" target="_blank"〉PubMed〈/a〉
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  • 10
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    Extreme ultraviolet observations from voyager 1 encounter with saturn (1981)
    American Association for the Advancement of Science (AAAS)
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    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〉
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