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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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    Titan's rotation reveals an internal ocean and changing zonal winds (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-03-22
    Description: Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present-day rotation period difference from synchronous spin leads to a shift of approximately 0.36 degrees per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating atmosphere, but only if Titan's crust is decoupled from the core by an internal water ocean like that on Europa.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lorenz, Ralph D -- Stiles, Bryan W -- Kirk, Randolph L -- Allison, Michael D -- Del Marmo, Paolo Persi -- Iess, Luciano -- Lunine, Jonathan I -- Ostro, Steven J -- Hensley, Scott -- Intramural NIH HHS/ -- New York, N.Y. -- Science. 2008 Mar 21;319(5870):1649-51. doi: 10.1126/science.1151639.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Department, Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ralph.lorenz@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18356521" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; Ice ; *Saturn ; Spacecraft ; *Water ; 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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  • 4
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    Rapid and extensive surface changes near Titan's equator: evidence of April showers (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-03-19
    Description: Although there is evidence that liquids have flowed on the surface at Titan's equator in the past, to date, liquids have only been confirmed on the surface at polar latitudes, and the vast expanses of dunes that dominate Titan's equatorial regions require a predominantly arid climate. We report the detection by Cassini's Imaging Science Subsystem of a large low-latitude cloud system early in Titan's northern spring and extensive surface changes (spanning more than 500,000 square kilometers) in the wake of this storm. The changes are most consistent with widespread methane rainfall reaching the surface, which suggests that the dry channels observed at Titan's low latitudes are carved by seasonal precipitation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Turtle, E P -- Perry, J E -- Hayes, A G -- Lorenz, R D -- Barnes, J W -- McEwen, A S -- West, R A -- Del Genio, A D -- Barbara, J M -- Lunine, J I -- Schaller, E L -- Ray, T L -- Lopes, R M C -- Stofan, E R -- New York, N.Y. -- Science. 2011 Mar 18;331(6023):1414-7. doi: 10.1126/science.1201063.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. elizabeth.turtle@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21415347" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; *Methane ; *Saturn ; Spacecraft
    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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  • 5
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    A 5-micron-bright spot on Titan: evidence for surface diversity (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-10-08
    Description: Observations from the Cassini Visual and Infrared Mapping Spectrometer show an anomalously bright spot on Titan located at 80 degrees W and 20 degrees S. This area is bright in reflected light at all observed wavelengths, but is most noticeable at 5 microns. The spot is associated with a surface albedo feature identified in images taken by the Cassini Imaging Science Subsystem. We discuss various hypotheses about the source of the spot, reaching the conclusion that the spot is probably due to variation in surface composition, perhaps associated with recent geophysical phenomena.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Barnes, Jason W -- Brown, Robert H -- Turtle, Elizabeth P -- McEwen, Alfred S -- Lorenz, Ralph D -- Janssen, Michael -- Schaller, Emily L -- Brown, Michael E -- Buratti, Bonnie J -- Sotin, Christophe -- Griffith, Caitlin -- Clark, Roger -- Perry, Jason -- Fussner, Stephanie -- Barbara, John -- West, Richard -- Elachi, Charles -- Bouchez, Antonin H -- Roe, Henry G -- Baines, Kevin H -- Bellucci, Giancarlo -- Bibring, Jean-Pierre -- Capaccioni, Fabrizio -- Cerroni, Priscilla -- Combes, Michel -- Coradini, Angioletta -- Cruikshank, Dale P -- Drossart, Pierre -- Formisano, Vittorio -- Jaumann, Ralf -- Langevin, Yves -- Matson, Dennis L -- McCord, Thomas B -- Nicholson, Phillip D -- Sicardy, Bruno -- New York, N.Y. -- Science. 2005 Oct 7;310(5745):92-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. jbarnes@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16210535" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Dry Ice ; Extraterrestrial Environment ; Ice ; Methane ; *Saturn ; Spacecraft ; Spectrum Analysis ; Temperature ; Water
    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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