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  • 1
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    Worldwide observations of remarkable deep-sea squids (2001)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2001-12-26
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Vecchione, M -- Young, R E -- Guerra, A -- Lindsay, D J -- Clague, D A -- Bernhard, J M -- Sager, W W -- Gonzalez, A F -- Rocha, F J -- Segonzac, M -- New York, N.Y. -- Science. 2001 Dec 21;294(5551):2505.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Marine Fisheries Service, Systematics Laboratory, National Museum of Natural History, Washington, DC 20560, USA. vecchione.michael@nmnh.si.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11752567" target="_blank"〉PubMed〈/a〉
    Keywords: Animals ; Decapodiformes/*anatomy & histology/classification/*physiology ; *Ecosystem ; Escape Reaction ; Locomotion ; Movement ; Oceans and Seas ; Seawater ; Videotape Recording
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Thermal Structure of Jupiter's Upper Atmosphere Derived from the Galileo Probe (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1997-04-04
    Description: Temperatures in Jupiter's atmosphere derived from Galileo Probe deceleration data increase from 109 kelvin at the 175-millibar level to 900 ± 40 kelvin at 1 nanobar, consistent with Voyager remote sensing data. Wavelike oscillations are present at all levels. Vertical wavelengths are 10 to 25 kilometers in the deep isothermal layer, which extends from 12 to 0.003 millibars. Above the 0.003-millibar level, only 90- to 270- kilometer vertical wavelengths survive, suggesting dissipation of wave energy as the probable source of upper atmosphere heating.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Seiff -- Kirk -- Knight -- Young -- Milos -- Venkatapathy -- Mihalov -- Blanchard -- Schubert -- New York, N.Y. -- Science. 1997 Apr 4;276(5309):102-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉A. Seiff, Department of Meteorology, San Jose State University Foundation and MS 245-1, Ames Research Center, Moffett Field, CA 94035, USA. D. B. Kirk, University of Oregon, 37465 Riverside Drive, Pleasant Hill, Oregon 97455, USA. T. C. D. Knight, 2370 S. Brentwood St., Lakewood, CO 80227, USA. L. A. Young, Center for Space Physics, Boston University, 725 Commonwealth Ave., Boston, Massachusetts 02215, USA. F. S. Milos, M.S. 234-1, Ames Research Center, NASA, Moffett Field, CA 94035, USA. E. Venkatapathy, Eloret Institute, MS 230-2, Ames Research Center, Moffett Field, CA 94035, USA. J. D. Mihalov and R. E. Young, MS 245-3, Ames Research Center, Moffett Field, CA 94035, USA. R. C. Blanchard, MS 408A, Langley Research Center, NASA, Hampton, VA 23681, USA. G. Schubert, Department of Earth and Space Sciences, University of California, Los Angeles, CA 90024, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9082977" 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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    Structure of the Atmosphere of Jupiter: Galileo Probe Measurements (1996)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1996-05-10
    Description: Temperatures and pressures measured by the Galileo probe during parachute descent into Jupiter's atmosphere essentially followed the dry adiabat between 0.41 and 24 bars, consistent with the absence of a deep water cloud and with the low water content found by the mass spectrometer. From 5 to 15 bars, lapse rates were slightly stable relative to the adiabat calculated for the observed H2/He ratio, which suggests that upward heat transport in that range is not attributable to simple radial convection. In the upper atmosphere, temperatures of 〉1000 kelvin at the 0.01-microbar level confirmed the hot exosphere that had been inferred from Voyager occultations. The thermal gradient increased sharply to 5 kelvin per kilometer at a reconstructed altitude of 350 kilometers, as was recently predicted. Densities at 1000 kilometers were 100 times those in the pre-encounter engineering model.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Seiff -- Kirk -- Knight -- Mihalov -- Blanchard -- Young -- Schubert -- von Zahn U -- Lehmacher -- Milos -- Wang -- New York, N.Y. -- Science. 1996 May 10;272(5263):844-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉A. Seiff, Department of Meteorology, San Jose State University, San Jose, CA 95192, USA. D. B. Kirk, 37465 Riverside Drive, Pleasant Hill, OR 97455, USA. T. C. D. Knight, 2370 South Brentwood Street, Lakewood, CO 80227, USA. J. D. Mihalov, R. E. Young, F. S. Milos, J. Wang, NASA Ames Research Center, Moffett Field, CA 94035, USA. R. C. Blanchard, NASA Langley Research Center, Hampton, VA 23681, USA. G. Schubert, Department of Earth and Space Science, University of California, Los Angeles, CA 90024, USA. U. von Zahn, Institut fur Atmospharenphysik, Universitat Rostock, D(0)-2565 Kuhlungsborn, Germany. G. Lehmacher, NASA 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/8662574" 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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  • 4
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    Galileo probe: in situ observations of Jupiter's atmosphere (1996)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1996-05-10
    Description: The Galileo probe performed the first in situ measurements of the atmosphere of Jupiter on 7 December 1995. The probe returned data until it reached a depth corresponding to an atmospheric pressure of approximately 24 bars. This report presents a brief overview of the origins and purpose of the mission. Science objectives, entry parameters and mission events, and results are described. The remaining reports address in more detail the individual experiments summarized here.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Young, R E -- Smith, M A -- Sobeck, C K -- New York, N.Y. -- Science. 1996 May 10;272(5263):837-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, CA 94035, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/8629015" target="_blank"〉PubMed〈/a〉
    Keywords: Ammonia/analysis ; *Atmosphere ; Carbon/analysis ; *Extraterrestrial Environment ; Helium/analysis ; *Jupiter ; Nitrogen/analysis ; Noble Gases/analysis ; Oxygen/analysis ; Sulfur/analysis ; Water/analysis
    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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  • 5
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    Bioluminescence in mesopelagic squid: diel color change during counterillumination (1980)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1980-06-13
    Description: Two species of mesopelagic squid greatly altered the color of their bio-luminescence during counterillumination. The color change was triggered by changes in water temperature corresponding to those normally encountered by these vertically migrating animals. These squid can probably conceal themselves under the different colors of downwelling light that they encounter in their day and night habitats.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Young, R E -- Mencher, F M -- New York, N.Y. -- Science. 1980 Jun 13;208(4449):1286-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17830814" 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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  • 6
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    Structure of the Atmosphere of Venus up to 110 Kilometers: Preliminary Results from the Four Pioneer Venus Entry Probes (1979)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1979-02-23
    Description: The four Pioneer Venus entry probes transmitted data of good quality on the structure of the atmosphere below the clouds. Contrast of the structure below an altitude of 50 kilometers at four widely separated locations was found to be no more than a few degrees Kelvin, with slightly warmer temperatures at 30 degrees south latitude than at 5 degrees or 60 degrees north. The atmosphere was stably stratified above 15 or 20 kilometers, indicating that the near-adiabatic state is maintained by the general circulation. The profiles move from near-adiabatic toward radiative equilibrium at altitudes above 40 kilometers. There appears to be a region of vertical convection above the dense cloud deck, which lies at 47.5 to 49 kilometers and at temperature levels near 360 K. The atmosphere is nearly isothermal around 100 kilometers (175 to 180 K) and appears to exhibit a sizable temperature wave between 60 and 70 kilometers. This is where the 4-day wind is believed to occur. The temperature wave may be related to some of the wavelike phenomena seen in Mariner 10 ultraviolet photographs.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Seiff, A -- Kirk, D B -- Sommer, S C -- Young, R E -- Blanchard, R C -- Juergens, D W -- Lepetich, J E -- Intrieri, P F -- Findlay, J T -- Derr, J S -- New York, N.Y. -- Science. 1979 Feb 23;203(4382):787-90.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17832998" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 7
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    Thermal contrast in the atmosphere of venus: initial appraisal from pioneer venus probe data (1979)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1979-07-06
    Description: The altitude profiles of temperature and pressure measured during the descent of the four Pioneer Venus probes show small contrast below the clouds but significant differences within the clouds at altitudes from 45 to 61 kilometers. At 60 kilometers, the probe which entered at 59.3 degrees north latitude sensed temperatures 25 K below those of the lower latitude probes, and a sizable difference persisted down to and slightly below the cloud base. It also sensed pressure below those of the other probes by as much as 49 millibars at a mean pressure of 200 millibars. The measured pressure differences are consistent with cyclostrophic balance of zonal winds ranging from 130 +/- 20 meters per second at 60 kilometers to 60 +/- 17 meters per second at 40 kilometers, with evidence in addition of a nonaxisymmetric component of the winds. The clouds were found to be 10 to 20 K warmer than the extended profiles of the lower atmosphere, and the middle cloud is convectively unstable. Both phenomena are attributed to the absorption of thermal radiation from below. Above the clouds, in the lower stratosphere, the lapse rate decreases abruptly to 3.5 K per kilometer, and a superimposed wave is evident. At 100 kilometers, the temperature is minimum, with a mean value of about 170 K.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Seiff, A -- Kirk, D B -- Young, R E -- Sommer, S C -- Blanchard, R C -- Findlay, J T -- Kelly, G M -- New York, N.Y. -- Science. 1979 Jul 6;205(4401):46-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17778897" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 8
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    Overview of VEGA Venus Balloon in Situ Meteorological Measurements (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    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〉
    Print ISSN: 0036-8075
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  • 9
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    VEGA Balloon Dynamics and Vertical Winds in the Venus Middle Cloud Region (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1986-03-21
    Description: The VEGA balloons provided a long-term record of vertical wind fluctuations in a planetary atmosphere other than Earth's. The vertical winds were calculated from the observed displacement of the balloon relative to its equilibrium float altitude. The winds were intermittent; a large burst lasted several hours, and the peak velocity was 3 meters per second.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Linkin, V M -- Kerzhanovich, V V -- Lipatov, A N -- Pichkadze, K M -- Shurupov, A A -- Terterashvili, A V -- Ingersoli, A P -- Crisp, D -- Grossman, A W -- Young, R E -- Seiff, A -- Ragent, B -- Blamont, J E -- Elson, L S -- Preston, R A -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1417-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748083" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 10
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    Thermal structure of the venus atmosphere in the middle cloud layer (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1986-03-21
    Description: Thermal structure measurements obtained by the two VEGA balloons show the Venus middle cloud layer to be generally adiabatic. Temperatures measured by the two balloons at locations roughly symmetric about the equator differed by about 6.5 kelvins at a given pressure. The VEGA-2 temperatures were about 2.5 kelvins cooler and those of VEGA-1 about 4 kelvins warmer than temperatures measured by the Pioneer Venus Large Probe at these levels. Data taken by the VEGA-2 lander as it passed through the middle cloud agreed with those of the VEGA-2 balloon. Study of individual frames of the balloon data suggests the presence of multiple discrete air masses that are internally adiabatic but lie on slightly different adiabats. These adiabats, for a given balloon, can differ in temperature by as much as 1 kelvin at a given pressure.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Linkin, V M -- Kerzhanovich, V V -- Lipatov, A N -- Shurupov, A A -- Seiff, A -- Ragent, B -- Young, R E -- Ingersoll, A P -- Crisp, D -- Elson, L S -- Preston, R A -- Blamont, J E -- New York, N.Y. -- Science. 1986 Mar 21;231(4744):1420-2.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748084" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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