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  • 1
    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
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  • 2
    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
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  • 3
    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
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  • 4
    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
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