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  • 1
    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
    Publication Date: 1994-12-16
    Description: In the course of 71 days in lunar orbit, from 19 February to 3 May 1994, the Clementine spacecraft acquired just under two million digital images of the moon at visible and infrared wavelengths. These data are enabling the global mapping of the rock types of the lunar crust and the first detailed investigation of the geology of the lunar polar regions and the lunar far side. In addition, laser-ranging measurements provided the first view of the global topographic figure of the moon. The topography of many ancient impact basins has been measured, and a global map of the thickness of the lunar crust has been derived from the topography and gravity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nozette, S -- Rustan, P -- Pleasance, L P -- Kordas, J F -- Lewis, I T -- Park, H S -- Priest, R E -- Horan, D M -- Regeon, P -- Lichtenberg, C L -- Shoemaker, E M -- Eliason, E M -- McEwen, A S -- Robinson, M S -- Spudis, P D -- Acton, C H -- Buratti, B J -- Duxbury, T C -- Baker, D N -- Jakosky, B M -- Blamont, J E -- Corson, M P -- Resnick, J H -- Rollins, C J -- Davies, M E -- Lucey, P G -- Malaret, E -- Massie, M A -- Pieters, C M -- Reisse, R A -- Simpson, R A -- Smith, D E -- Sorenson, T C -- Breugge, R W -- Zuber, M T -- New York, N.Y. -- Science. 1994 Dec 16;266(5192):1835-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17737076" target="_blank"〉PubMed〈/a〉
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  • 3
    Publication Date: 2010-05-08
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gleick, P H -- Adams, R M -- Amasino, R M -- Anders, E -- Anderson, D J -- Anderson, W W -- Anselin, L E -- Arroyo, M K -- Asfaw, B -- Ayala, F J -- Bax, A -- Bebbington, A J -- Bell, G -- Bennett, M V L -- Bennetzen, J L -- Berenbaum, M R -- Berlin, O B -- Bjorkman, P J -- Blackburn, E -- Blamont, J E -- Botchan, M R -- Boyer, J S -- Boyle, E A -- Branton, D -- Briggs, S P -- Briggs, W R -- Brill, W J -- Britten, R J -- Broecker, W S -- Brown, J H -- Brown, P O -- Brunger, A T -- Cairns, J Jr -- Canfield, D E -- Carpenter, S R -- Carrington, J C -- Cashmore, A R -- Castilla, J C -- Cazenave, A -- Chapin, F S 3rd -- Ciechanover, A J -- Clapham, D E -- Clark, W C -- Clayton, R N -- Coe, M D -- Conwell, E M -- Cowling, E B -- Cowling, R M -- Cox, C S -- Croteau, R B -- Crothers, D M -- Crutzen, P J -- Daily, G C -- Dalrymple, G B -- Dangl, J L -- Darst, S A -- Davies, D R -- Davis, M B -- De Camilli, P V -- Dean, C -- DeFries, R S -- Deisenhofer, J -- Delmer, D P -- DeLong, E F -- DeRosier, D J -- Diener, T O -- Dirzo, R -- Dixon, J E -- Donoghue, M J -- Doolittle, R F -- Dunne, T -- Ehrlich, P R -- Eisenstadt, S N -- Eisner, T -- Emanuel, K A -- Englander, S W -- Ernst, W G -- Falkowski, P G -- Feher, G -- Ferejohn, J A -- Fersht, A -- Fischer, E H -- Fischer, R -- Flannery, K V -- Frank, J -- Frey, P A -- Fridovich, I -- Frieden, C -- Futuyma, D J -- Gardner, W R -- Garrett, C J R -- Gilbert, W -- Goldberg, R B -- Goodenough, W H -- Goodman, C S -- Goodman, M -- Greengard, P -- Hake, S -- Hammel, G -- Hanson, S -- Harrison, S C -- Hart, S R -- Hartl, D L -- Haselkorn, R -- Hawkes, K -- Hayes, J M -- Hille, B -- Hokfelt, T -- House, J S -- Hout, M -- Hunten, D M -- Izquierdo, I A -- Jagendorf, A T -- Janzen, D H -- Jeanloz, R -- Jencks, C S -- Jury, W A -- Kaback, H R -- Kailath, T -- Kay, P -- Kay, S A -- Kennedy, D -- Kerr, A -- Kessler, R C -- Khush, G S -- Kieffer, S W -- Kirch, P V -- Kirk, K -- Kivelson, M G -- Klinman, J P -- Klug, A -- Knopoff, L -- Kornberg, H -- Kutzbach, J E -- Lagarias, J C -- Lambeck, K -- Landy, A -- Langmuir, C H -- Larkins, B A -- Le Pichon, X T -- Lenski, R E -- Leopold, E B -- Levin, S A -- Levitt, M -- Likens, G E -- Lippincott-Schwartz, J -- Lorand, L -- Lovejoy, C O -- Lynch, M -- Mabogunje, A L -- Malone, T F -- Manabe, S -- Marcus, J -- Massey, D S -- McWilliams, J C -- Medina, E -- Melosh, H J -- Meltzer, D J -- Michener, C D -- Miles, E L -- Mooney, H A -- Moore, P B -- Morel, F M M -- Mosley-Thompson, E S -- Moss, B -- Munk, W H -- Myers, N -- Nair, G B -- Nathans, J -- Nester, E W -- Nicoll, R A -- Novick, R P -- O'Connell, J F -- Olsen, P E -- Opdyke, N D -- Oster, G F -- Ostrom, E -- Pace, N R -- Paine, R T -- Palmiter, R D -- Pedlosky, J -- Petsko, G A -- Pettengill, G H -- Philander, S G -- Piperno, D R -- Pollard, T D -- Price, P B Jr -- Reichard, P A -- Reskin, B F -- Ricklefs, R E -- Rivest, R L -- Roberts, J D -- Romney, A K -- Rossmann, M G -- Russell, D W -- Rutter, W J -- Sabloff, J A -- Sagdeev, R Z -- Sahlins, M D -- Salmond, A -- Sanes, J R -- Schekman, R -- Schellnhuber, J -- Schindler, D W -- Schmitt, J -- Schneider, S H -- Schramm, V L -- Sederoff, R R -- Shatz, C J -- Sherman, F -- Sidman, R L -- Sieh, K -- Simons, E L -- Singer, B H -- Singer, M F -- Skyrms, B -- Sleep, N H -- Smith, B D -- Snyder, S H -- Sokal, R R -- Spencer, C S -- Steitz, T A -- Strier, K B -- Sudhof, T C -- Taylor, S S -- Terborgh, J -- Thomas, D H -- Thompson, L G -- Tjian, R T -- Turner, M G -- Uyeda, S -- Valentine, J W -- Valentine, J S -- Van Etten, J L -- van Holde, K E -- Vaughan, M -- Verba, S -- von Hippel, P H -- Wake, D B -- Walker, A -- Walker, J E -- Watson, E B -- Watson, P J -- Weigel, D -- Wessler, S R -- West-Eberhard, M J -- White, T D -- Wilson, W J -- Wolfenden, R V -- Wood, J A -- Woodwell, G M -- Wright, H E Jr -- Wu, C -- Wunsch, C -- Zoback, M L -- Howard Hughes Medical Institute/ -- New York, N.Y. -- Science. 2010 May 7;328(5979):689-90. doi: 10.1126/science.328.5979.689.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20448167" target="_blank"〉PubMed〈/a〉
    Keywords: *Climate Change ; Politics ; Public Policy ; Research/standards ; Research Personnel
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  • 4
    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
    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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  • 6
    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〉
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  • 7
    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
    Publication Date: 1986-03-21
    Description: The VEGA Venus balloon radio transmissions received on Earth were used to measure the motion of the balloons and to obtain the data recorded by onboard sensors measuring atmospheric characteristics. Thus the balloons themselves, the gondolas, the onboard sensors, and the radio transmission system were all components of the experiment. A description of these elements is given, and a few details of data sampling and formatting are discussed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kremnev, R S -- Linkin, V M -- Lipatov, A N -- Pichkadze, K M -- Shurupov, A A -- Terterashvili, A V -- Bakitko, R V -- Blamont, J E -- Malique, C -- Ragent, B -- Preston, R A -- Elson, L S -- Crisp, D -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1408-11.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748080" target="_blank"〉PubMed〈/a〉
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  • 9
    Publication Date: 1986-03-21
    Description: The VEGA balloons made in situ measurements of pressure, temperature, vertical wind velocity, ambient light, frequency of lightning, and cloud particle backscatter. Both balloons encountered highly variable atmospheric conditions, with periods of intense vertical winds occurring sporadically throughout their flights. Downward winds as large as 3.5 meters per second occasionally forced the balloons to descend as much as 2.5 kilometers below their equilibrium float altitudes. Large variations, in pressure, temperature, ambient light level, and cloud particle backscatter (VEGA-1 only) correlated well during these excursions, indicating that these properties were strong functions of altitude in those parts of the middle cloud layer sampled by the balloons.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sagdeev, R Z -- Linkin, V M -- Kerzhanovich, V V -- Lipatov, A N -- Shurupov, A A -- Blamont, J E -- Crisp, D -- Ingersoll, A P -- Elson, L S -- Preston, R A -- Hildebrand, C E -- Ragent, B -- Seiff, A -- Young, R E -- Petit, G -- Boloh, L -- Alexandrov, Y N -- Armand, N A -- Bakitko, R V -- Selivanov, A S -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1411-4.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748081" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 1986-03-21
    Description: A global array of 20 radio observatories was used to measure the three-dimensional position and velocity of the two meteorological balloons that were injected into the equatorial region of the Venus atmosphere near Venus midnight by the VEGA spacecraft on 11 and 15 June 1985. Initial analysis of only radial velocities indicates that each balloon was blown westward about 11,500 kilometers (8,000 kilometers on the night side) by zonal winds with a mean speed of about 70 meters per second. Excursions of the data from a model of constant zonal velocity were generally less than 3 meters per second; however, a much larger variation was evident near the end of the flight of the second balloon. Consistent systematic trends in the residuals for both balloons indicate the possibility of a solar-fixed atmospheric feature. Rapid variations in balloon velocity were often detected within a single transmission (330 seconds); however, they may represent not only atmospheric motions but also self-induced aerodynamic motions of the balloon.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Preston, R A -- Hildebrand, C E -- Purcell, G H Jr -- Ellis, J -- Stelzried, C T -- Finley, S G -- Sagdeev, R Z -- Linkin, V M -- Kerzhanovich, V V -- Altunin, V I -- Kogan, L R -- Kostenko, V I -- Matveenko, L I -- Pogrebenko, S V -- Strukov, I A -- Akim, E L -- Alexandrov, Y N -- Armand, N A -- Bakitko, R N -- Vyshlov, A S -- Bogomolov, A F -- Gorchankov, Y N -- Selivanov, A S -- Ivanov, N M -- Tichonov, V F -- Blamont, J E -- Boloh, L -- Laurans, G -- Boischot, A -- Biraud, F -- Ortega-Molina, A -- Rosolen, C -- Petit, G -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1414-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748082" target="_blank"〉PubMed〈/a〉
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