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  • 1
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    Planetary science. The weather on Titan (2001)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2001-02-24
    Description: When the Voyager 1 spacecraft returned images in 1980, the dense atmosphere of Saturn's moon Titan was assumed to be bland and featureless. As Lorenz discusses in his Perspective, recent ground-based spectroscopy, and images from the Hubble Space Telescope, are changing this perception. Observations such as the short-lived clouds in Titan's atmosphere reported by Griffith et al. suggest that although average precipitation is likely to be low, individual precipitation events may be heavy enough to cause deep valleys on Titan's surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lorenz, R D -- New York, N.Y. -- Science. 2000 Oct 20;290(5491):467-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, 85721, USA. rlorenz@pl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11183770" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment ; Methane ; Rain ; *Saturn ; Temperature ; Thermodynamics ; Water ; Weather
    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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    Photochemically driven collapse of Titan's atmosphere (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1997-01-31
    Description: Saturn's giant moon Titan has a thick (1.5 bar) nitrogen atmosphere, which has a temperature structure that is controlled by the absorption of solar and thermal radiation by methane, hydrogen, and organic aerosols into which methane is irreversibly converted by photolysis. Previous studies of Titan's climate evolution have been done with the assumption that the methane abundance was maintained against photolytic depletion throughout Titan's history, either by continuous supply from the interior or by buffering by a surface or near surface reservoir. Radiative-convective and radiative-saturated equilibrium models of Titan's atmosphere show that methane depletion may have allowed Titan's atmosphere to cool so that nitrogen, its main constituent, condenses onto the surface, collapsing Titan into a Triton-like frozen state with a thin atmosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lorenz, R D -- McKay, C P -- Lunine, J I -- New York, N.Y. -- Science. 1997 Jan 31;275(5300):642-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Planetary Sciences, Lunar and Planetary Laboratory, University of Arizona, Tucson 85721, USA.rlorenz@pl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9005844" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Evolution, Planetary ; *Extraterrestrial Environment ; *Methane ; *Nitrogen ; Photolysis ; *Saturn ; Temperature
    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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  • 3
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    The sand seas of Titan: Cassini RADAR observations of longitudinal dunes (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-05-06
    Description: The most recent Cassini RADAR images of Titan show widespread regions (up to 1500 kilometers by 200 kilometers) of near-parallel radar-dark linear features that appear to be seas of longitudinal dunes similar to those seen in the Namib desert on Earth. The Ku-band (2.17-centimeter wavelength) images show approximately 100-meter ridges consistent with duneforms and reveal flow interactions with underlying hills. The distribution and orientation of the dunes support a model of fluctuating surface winds of approximately 0.5 meter per second resulting from the combination of an eastward flow with a variable tidal wind. The existence of dunes also requires geological processes that create sand-sized (100- to 300-micrometer) particulates and a lack of persistent equatorial surface liquids to act as sand traps.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lorenz, R D -- Wall, S -- Radebaugh, J -- Boubin, G -- Reffet, E -- Janssen, M -- Stofan, E -- Lopes, R -- Kirk, R -- Elachi, C -- Lunine, J -- Mitchell, K -- Paganelli, F -- Soderblom, L -- Wood, C -- Wye, L -- Zebker, H -- Anderson, Y -- Ostro, S -- Allison, M -- Boehmer, R -- Callahan, P -- Encrenaz, P -- Ori, G G -- Francescetti, G -- Gim, Y -- Hamilton, G -- Hensley, S -- Johnson, W -- Kelleher, K -- Muhleman, D -- Picardi, G -- Posa, F -- Roth, L -- Seu, R -- Shaffer, S -- Stiles, B -- Vetrella, S -- Flamini, E -- West, R -- New York, N.Y. -- Science. 2006 May 5;312(5774):724-7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. rlorenz@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16675695" target="_blank"〉PubMed〈/a〉
    Keywords: *Extraterrestrial Environment ; Geologic Sediments ; Hydrocarbons/chemistry ; Methane/chemistry ; Particle Size ; Radar ; *Saturn ; Spacecraft ; Wind
    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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