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  • American Association for the Advancement of Science (AAAS)  (3,906)
  • 1985-1989  (2,096)
  • 1980-1984  (1,810)
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  • 1
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    Voyager 2 at neptune: imaging science results (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-12-15
    Description: Voyager 2 images of Neptune reveal a windy planet characterized by bright clouds of methane ice suspended in an exceptionally clear atmosphere above a lower deck of hydrogen sulfide or ammonia ices. Neptune's atmosphere is dominated by a large anticyclonic storm system that has been named the Great Dark Spot (GDS). About the same size as Earth in extent, the GDS bears both many similarities and some differences to the Great Red Spot of Jupiter. Neptune's zonal wind profile is remarkably similar to that of Uranus. Neptune has three major rings at radii of 42,000, 53,000, and 63,000 kilometers. The outer ring contains three higher density arc-like segments that were apparently responsible for most of the ground-based occultation events observed during the current decade. Like the rings of Uranus, the Neptune rings are composed of very dark material; unlike that of Uranus, the Neptune system is very dusty. Six new regular satellites were found, with dark surfaces and radii ranging from 200 to 25 kilometers. All lie inside the orbit of Triton and the inner four are located within the ring system. Triton is seen to be a differentiated body, with a radius of 1350 kilometers and a density of 2.1 grams per cubic centimeter; it exhibits clear evidence of early episodes of surface melting. A now rigid crust of what is probably water ice is overlain with a brilliant coating of nitrogen frost, slightly darkened and reddened with organic polymer material. Streaks of organic polymer suggest seasonal winds strong enough to move particles of micrometer size or larger, once they become airborne. At least two active plumes were seen, carrying dark material 8 kilometers above the surface before being transported downstream by high level winds. The plumes may be driven by solar heating and the subsequent violent vaporization of subsurface nitrogen.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, B A -- Soderblom, L A -- Banfield, D -- Barnet, C -- Basilevsky, A T -- Beebe, R F -- Bollinger, K -- Boyce, J M -- Brahic, A -- Briggs, G A -- Brown, R H -- Chyba, C -- Collins, S A -- Colvin, T -- Cook, A F 2nd -- Crisp, D -- Croft, S K -- Cruikshank, D -- Cuzzi, J N -- Danielson, G E -- Davies, M E -- De Jong, E -- Dones, L -- Godfrey, D -- Goguen, J -- Grenier, I -- Haemmerle, V R -- Hammel, H -- Hansen, C J -- Helfenstein, C P -- Howell, C -- Hunt, G E -- Ingersoll, A P -- Johnson, T V -- Kargel, J -- Kirk, R -- Kuehn, D I -- Limaye, S -- Masursky, H -- McEwen, A -- Morrison, D -- Owen, T -- Owen, W -- Pollack, J B -- Porco, C C -- Rages, K -- Rogers, P -- Rudy, D -- Sagan, C -- Schwartz, J -- Shoemaker, E M -- Showalter, M -- Sicardy, B -- Simonelli, D -- Spencer, J -- Sromovsky, L A -- Stoker, C -- Strom, R G -- Suomi, V E -- Synott, S P -- Terrile, R J -- Thomas, P -- Thompson, W R -- Verbiscer, A -- Veverka, J -- New York, N.Y. -- Science. 1989 Dec 15;246(4936):1422-49.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17755997" target="_blank"〉PubMed〈/a〉
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  • 2
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    Cloned viral protein vaccine for foot-and-mouth disease: responses in cattle and swine (1981)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1981-12-04
    Description: A DNA sequence coding for the immunogenic capsid protein VP3 of foot-and-mouth disease virus A12, prepared from the virion RNA, was ligated to a plasmid designed to express a chimeric protein from the Escherichia coli tryptophan promoter-operator system. When Escherichia coli transformed with this plasmid was grown in tryptophan-depleted media, approximately 17 percent of the total cellular protein was found to be an insoluble and stable chimeric protein. The purified chimeric protein competed equally on a molar basis with VP3 for specific antibodies to foot-and-mouth disease virus. When inoculated into six cattle and two swine, this protein elicited high levels of neutralizing antibody and protection against challenge with foot-and-mouth disease virus.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kleid, D G -- Yansura, D -- Small, B -- Dowbenko, D -- Moore, D M -- Grubman, M J -- McKercher, P D -- Morgan, D O -- Robertson, B H -- Bachrach, H L -- New York, N.Y. -- Science. 1981 Dec 4;214(4525):1125-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/6272395" target="_blank"〉PubMed〈/a〉
    Keywords: Amino Acid Sequence ; Animals ; Antibody Formation ; Base Sequence ; Cattle ; Cattle Diseases/*prevention & control ; *Cloning, Molecular ; DNA Restriction Enzymes ; DNA, Recombinant/metabolism ; Foot-and-Mouth Disease/*prevention & control ; Immunity, Cellular ; Protein Biosynthesis ; Swine ; Swine Diseases/*prevention & control ; Transcription, Genetic ; *Vaccines ; Viral Proteins/genetics/*therapeutic use
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  • 3
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    Plea to the scientific community (1982)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1982-06-04
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Baltimore, D -- Berg, P -- Bloch, K E -- Brown, D D -- Kornberg, A -- Nathans, D -- Smith, H O -- Watson, J D -- Thomas, L -- New York, N.Y. -- Science. 1982 Jun 4;216(4550):1046.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17808459" target="_blank"〉PubMed〈/a〉
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  • 4
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    Hayflick-NIH Settlement (1982)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1982-01-15
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Strehler, B L -- Abraham, S -- Bayreuther, K -- Bienenstock, A -- Binstock, R -- Birren, J -- Blumenthal, H T -- Brautbar, C -- Brody, E M -- Brody, H -- Comfort, A -- Cottle, R W -- Danielli, J F -- Danon, D -- Datan, N -- Ebbesen, P -- Elsen, A -- Freundt, E A -- Gallop, P M -- Girardi, A J -- Glenn, P F -- Goheen, J D -- Goldstein, S -- Good, R A -- Goodlin, R C -- Granoff, A -- Gray, A -- Haber, P A -- Hamparian, V V -- Hijmans, W -- Holliday, R -- Horvath, S M -- Houck, J C -- Huebner, R J -- Itoh, H -- Jukes, T -- Kaplan, H S -- Kirkman, H -- Kuwert, E -- Leiderman, P H -- Liss, A -- Litwin, J -- Lubin, B -- Macieira-Coelho, A -- Madoff, S -- Maletta, G J -- Maramorosch, K -- Martin, G M -- Masover, G -- Matsumura, T -- Medvedev, Z -- Melnick, J L -- Merchant, D J -- Namba, M -- Neter, E -- Neugarten, B -- Orgel, L -- Outschoorn, A S -- Pace, D M -- Packer, L -- Parker, J C -- Patterson, M D Jr -- Pollard, M -- Portnuff, J -- Razin, S -- Reiff, T R -- Robert, L -- Rockstein, M -- Rosamoff, H -- Rosanoff, E I -- Rottem, S -- Schachter, J -- Schwartz, H -- Shanas, E -- Shimkin, M B -- Smith, J R -- Somerson, N L -- Stinebring, W -- Textor, R -- Thomas, L -- Viidik, A -- Weg, R -- Yabrov, A -- Yanofsky, C -- Zatz, L M -- New York, N.Y. -- Science. 1982 Jan 15;215(4530):240-2.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17784330" target="_blank"〉PubMed〈/a〉
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  • 5
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    A Comparison of SIR-B Directional Ocean Wave Spectra with Aircraft Scanning Radar Spectra (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1986-06-20
    Description: Directional ocean wave spectra derived from Shuttle Imaging Radar-B (SIR-B) L-band imagery collected off the coast of southern Chile on 11 and 12 October 1984 were compared with independent spectral estimates from two airborne scanning radars. In sea states with significant wave heights ranging from 3 to 5 meters, the SIR-B-derived spectra at 18 degrees and 25 degrees off nadir yielded reasonable estimates of wavelengths, directions, and spectral shapes for all wave systems encountered, including a purely azimuth-traveling system. A SIR-B image intensity variance spectrum containing predominantly range-traveling waves closely resembles an independent aircraft estimate of the slope variance spectrum. The prediction of a U.S. Navy global spectral ocean wave model on 11 October 1984 exhibited no significant bias in dominant wave number but contained a directional bias of about 30 degrees espect to the mean of the aircraft and spacecraft estimates.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Beal, R C -- Monaldo, F M -- Tilley, D G -- Irvine, D E -- Walsh, E J -- Jackson, F C -- Hancock, D W 3rd -- Hines, D E -- Swift, R N -- Gonzalez, F L -- Lyzenga, D R -- Zambresky, L F -- New York, N.Y. -- Science. 1986 Jun 20;232(4757):1531-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17773503" target="_blank"〉PubMed〈/a〉
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  • 6
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    Absence of linkage of chromosome 21q21 markers to familial Alzheimer's disease (1988)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1988-09-16
    Description: Alzheimer's disease is the most common form of dementia among the elderly population. Although the etiology is unknown, inheritance plays a role in the pathogenesis of the disease. Recent work indicates that an autosomal dominant gene for Alzheimer's disease is located on chromosome 21 at band q21. In the present study of a group of autopsy-documented kindreds, no evidence for linkage was found between familial Alzheimer's disease (FAD) and chromosome 21q21 markers (D21S1/D21S72 and the amyloid beta gene). Linkage to the D21S1/D21S72 locus was excluded at recombination fractions (theta) up to 0.17. Linkage to the amyloid gene was excluded at theta = 0.10. Apparent recombinants were noted in two families for the amyloid gene and in five families for the D21S1/D21S72 locus. These data indicate that FAD is genetically heterogeneous.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Schellenberg, G D -- Bird, T D -- Wijsman, E M -- Moore, D K -- Boehnke, M -- Bryant, E M -- Lampe, T H -- Nochlin, D -- Sumi, S M -- Deeb, S S -- AG 00057/AG/NIA NIH HHS/ -- AG 05136/AG/NIA NIH HHS/ -- GM 15253/GM/NIGMS NIH HHS/ -- New York, N.Y. -- Science. 1988 Sep 16;241(4872):1507-10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Division of Neurology, University of Washington, Seattle 98195.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/3420406" target="_blank"〉PubMed〈/a〉
    Keywords: Alzheimer Disease/*genetics ; Chromosome Mapping ; *Chromosomes, Human, Pair 21 ; Genetic Linkage ; Humans
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  • 7
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    Ecological effects of a major oil spill on panamanian coastal marine communities (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-01-06
    Description: In 1986 more than 8 million liters of crude oil spilled into a complex region of mangroves, seagrasses, and coral reefs just east of the Caribbean entrance to the Panama Canal. This was the largest recorded spill into coastal habitats in the tropical Americas. Many population of plants and animals in both oiled and unoiled sites had been studied previously, thereby providing an unprecedented measure of ecological variation before the spill. Documenation of the spread of oil and its biological begun immediately. Intertidal mangroves, algae, and associated invertebrates were covered by oil and died soon after. More surprisingly, there was also extensive mortality of shallow subtidal reef corals and infauna of seagrass beds. After 1.5 years only some organisms in areas exposed to the open sea have recovered.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jackson, J B -- Cubit, J D -- Keller, B D -- Batista, V -- Burns, K -- Caffey, H M -- Caldwell, R L -- Garrity, S D -- Getter, C D -- Gonzalez, C -- Guzman, H M -- Kaufmann, K W -- Knap, A H -- Levings, S C -- Marshall, M J -- Steger, R -- Thompson, R C -- Weil, E -- New York, N.Y. -- Science. 1989 Jan 6;243(4887):37-44.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17780421" target="_blank"〉PubMed〈/a〉
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  • 8
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    Voyager planetary radio astronomy at neptune (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-12-15
    Description: Detection of very intense short radio bursts from Neptune was possible as early as 30 days before closest approach and at least 22 days after closest approach. The bursts lay at frequencies in the range 100 to 1300 kilohertz, were narrowband and strongly polarized, and presumably originated in southern polar regions ofthe planet. Episodes of smooth emissions in the frequency range from 20 to 865 kilohertz were detected during an interval of at least 10 days around closest approach. The bursts and the smooth emissions can be described in terms of rotation in a period of 16.11 +/- 0.05 hours. The bursts came at regular intervals throughout the encounter, including episodes both before and after closest approach. The smooth emissions showed a half-cycle phase shift between the five episodes before and after closest approach. This experiment detected the foreshock of Neptune's magnetosphere and the impacts of dust at the times of ring-plane crossings and also near the time of closest approach. Finally, there is no evidence for Neptunian electrostatic discharges.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Warwick, J W -- Evans, D R -- Peltzer, G R -- Peltzer, R G -- Romig, J H -- Sawyer, C B -- Riddle, A C -- Schweitzer, A E -- Desch, M D -- Kaiser, M L -- Farrell, W M -- Carr, T D -- de Pater, I -- Staelin, D H -- Gulkis, S -- Poynter, R L -- Boischot, A -- Genova, F -- Leblanc, Y -- Lecacheux, A -- Pedersen, B M -- Zarka, P -- New York, N.Y. -- Science. 1989 Dec 15;246(4936):1498-501.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17756007" target="_blank"〉PubMed〈/a〉
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  • 9
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    Voyager radio science observations of neptune and triton (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-12-15
    Description: The Voyager 2 encounter with the Neptune system included radio science investigations of the masses and densities of Neptune and Triton, the low-order gravitational harmonics of Neptune, the vertical structures of the atmospheres and ionospheres of Neptune and Triton, the composition of the atmosphere of Neptune, and characteristics of ring material. Demanding experimental requirements were met successfully, and study of the large store of collected data has begun. The initial search of the data revealed no detectable effects of ring material with optical depth tau [unknown] 0.01. Preliminary representative results include the following: 1.0243 x 10(26) and 2.141 x 10(22) kilograms for the masses of Neptune and Triton; 1640 and 2054 kilograms per cubic meter for their respective densities; 1355 +/- 7 kilometers, provisionally, for the radius of Triton; and J(2) = 3411 +/- 10(x 10(-6)) and J(4) = -26(+12)(-20)(x10(-6)) for Neptune's gravity field (J〉(2) and J(4) are harmonic coefficients of the gravity field). The equatorial and polar radii of Neptune are 24,764 +/- 20 and 24,340 +/- 30 kllometers, respectively, at the 10(5)-pascal (1 bar) pressure level. Neptune's atmosphere was probed to a pressure level of about 5 x 10(5) pascals, and effects of a methane cloud region and probable ammonia absorption below the cloud are evident in the data. Results for the mixing ratios of helium and ammonia are still being investigated; the methane abundance below the clouds is at least 1 percent by volume. Derived temperature-pressure profiles to 1.2 x 10(5) pascals and 78 kelvins (K) show a lapse rate corresponding to "frozen" equilibrium of the para- and ortho-hydrogen states. Neptune's ionosphere exhibits an extended topside at a temperature of 950 +/- 160 K if H(+) is the dominant ion, and narrow ionization layers of the type previously seen at the other three giant planets. Triton has a dense ionosphere with a peak electron concentration of 46 x 10(9) per cubic meter at an altitude of 340 kilometers measured during occultation egress. Its topside plasma temperature is about 80 +/- 16 K if N(2)(+) is the principal ion. The tenuous neutral atmosphere of Triton produced distinct signatures in the occultation data; however, the accuracy of the measurements is limited by uncertainties in the frequency of the spacecraft reference oscillator. Preliminary values for the surface pressure of 1.6 +/- 0.3 pascals and an equivalent isothermal temperature of 48 +/- 5 K are suggested, on the assumption that molecular nitrogen dominates the atmosphere. The radio data may be showing the effects of a thermal inversion near the surface; this and other evidence imply that the Triton atmosphere is controlled by vapor-pressure equilibrium with surface ices, at a temperature of 38 K and a methane mixing ratio of about 10(-4).〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Tyler, G L -- Sweetnam, D N -- Anderson, J D -- Borutzki, S E -- Campbell, J K -- Eshleman, V R -- Gresh, D L -- Gurrola, E M -- Hinson, D P -- Kawashima, N -- Kursinski, E R -- Levy, G S -- Lindal, G F -- Lyons, J R -- Marouf, E A -- Rosen, P A -- Simpson, R A -- Wood, G E -- New York, N.Y. -- Science. 1989 Dec 15;246(4936):1466-73.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17756001" target="_blank"〉PubMed〈/a〉
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  • 10
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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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