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  • 1
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    American Association for the Advancement of Science (AAAS)
    Publication Date: 2000-05-20
    Description: Unlike any volcanic behavior ever observed on Earth, the plume from Prometheus on Io has wandered 75 to 95 kilometers west over the last 20 years since it was first discovered by Voyager and more recently observed by Galileo. Despite the source motion, the geometric and optical properties of the plume have remained constant. We propose that this can be explained by vaporization of a sulfur dioxide and/or sulfur "snowfield" over which a lava flow is moving. Eruption of a boundary-layer slurry through a rootless conduit with sonic conditions at the intake of the melted snow can account for the constancy of plume properties.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kieffer, S W -- Lopes-Gautier, R -- McEwen, A -- Smythe, W -- Keszthelyi, L -- Carlson, R -- New York, N.Y. -- Science. 2000 May 19;288(5469):1204-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉S. W. Kieffer Science Consulting, Inc., 6 Queen Street, Suite 206, Post Office Box 520, Bolton, ON L7E 5T4, Canada. skieffer@geyser.com〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10817989" target="_blank"〉PubMed〈/a〉
    Keywords: Cold Temperature ; Entropy ; Extraterrestrial Environment ; Hot Temperature ; Ice ; *Jupiter ; Models, Chemical ; Snow ; Spacecraft ; *Volcanic Eruptions
    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: 1998-03-28
    Description: High-resolution images of the martian surface at scales of a few meters show ubiquitous erosional and depositional eolian landforms. Dunes, sandsheets, and drifts are prevalent and exhibit a range of morphology, composition (inferred from albedo), and age (as seen in occurrences of different dune orientations at the same location). Steep walls of topographic depressions such as canyons, valleys, and impact craters show the martian crust to be stratified at scales of a few tens of meters. The south polar layered terrain and superposed permanent ice cap display diverse surface textures that may reflect the complex interplay of volatile and non-volatile components. Low resolution regional views of the planet provide synoptic observations of polar cap retreat, condensate clouds, and the lifecycle of local and regional dust storms.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Malin, M C -- Carr, M H -- Danielson, G E -- Davies, M E -- Hartmann, W K -- Ingersoll, A P -- James, P B -- Masursky, H -- McEwen, A S -- Soderblom, L A -- Thomas, P -- Veverka, J -- Caplinger, M A -- Ravine, M A -- Soulanille, T A -- Warren, J L -- New York, N.Y. -- Science. 1998 Mar 13;279(5357):1681-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Malin Space Science Systems, Post Office Box 910148, San Diego, CA 92191-0148, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9497280" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Dioxide ; *Extraterrestrial Environment ; Ice ; *Mars ; 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: 2005-02-26
    Description: The Cassini Imaging Science Subsystem acquired high-resolution imaging data on the outer Saturnian moon, Phoebe, during Cassini's close flyby on 11 June 2004 and on Iapetus during a flyby on 31 December 2004. Phoebe has a heavily cratered and ancient surface, shows evidence of ice near the surface, has distinct layering of different materials, and has a mean density that is indicative of an ice-rock mixture. Iapetus's dark leading side (Cassini Regio) is ancient, heavily cratered terrain bisected by an equatorial ridge system that reaches 20 kilometers relief. Local albedo variations within and bordering Cassini Regio suggest mass wasting of ballistically deposited material, the origin of which remains unknown.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Porco, C C -- Baker, E -- Barbara, J -- Beurle, K -- Brahic, A -- Burns, J A -- Charnoz, S -- Cooper, N -- Dawson, D D -- Del Genio, A D -- Denk, T -- Dones, L -- Dyudina, U -- Evans, M W -- Giese, B -- Grazier, K -- Helfenstein, P -- Ingersoll, A P -- Jacobson, R A -- Johnson, T V -- McEwen, A -- Murray, C D -- Neukum, G -- Owen, W M -- Perry, J -- Roatsch, T -- Spitale, J -- Squyres, S -- Thomas, P C -- Tiscareno, M -- Turtle, E -- Vasavada, A R -- Veverka, J -- Wagner, R -- West, R -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1237-42.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Cassini Imaging Central Laboratory for Operations, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA. carolyn@ciclops.org〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731440" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geologic Sediments ; Ice ; *Saturn ; Spacecraft ; 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: 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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  • 5
    Publication Date: 2007-09-22
    Description: Mars' north pole is covered by a dome of layered ice deposits. Detailed ( approximately 30 centimeters per pixel) images of this region were obtained with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter (MRO). Planum Boreum basal unit scarps reveal cross-bedding and show evidence for recent mass wasting, flow, and debris accumulation. The north polar layers themselves are as thin as 10 centimeters but appear to be covered by a dusty veneer in places, which may obscure thinner layers. Repetition of particular layer types implies that quasi-periodic climate changes influenced the stratigraphic sequence in the polar layered deposits, informing models for recent climate variations on Mars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Herkenhoff, K E -- Byrne, S -- Russell, P S -- Fishbaugh, K E -- McEwen, A S -- New York, N.Y. -- Science. 2007 Sep 21;317(5845):1711-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astrogeology Team, United States Geological Survey (USGS), Flagstaff, AZ 86001, USA. kherkenhoff@usgs.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17885127" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Ice ; *Mars
    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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