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  • 1
    Publication Date: 2004-12-18
    Description: Neutral oxygen in the saturnian system shows variability, and the total number of oxygen atoms peaks at 4 x 10(34). Saturn's aurora brightens in response to solar-wind forcing, and the auroral spectrum resembles Jupiter's. Phoebe's surface shows variable water-ice content, and the data indicate it originated in the outer solar system. Saturn's rings also show variable water abundance, with the purest ice in the outermost A ring. This radial variation is consistent with initially pure water ice bombarded by meteors, but smaller radial structures may indicate collisional transport and recent renewal events in the past 10(7) to 10(8) years.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Esposito, Larry W -- Colwell, Joshua E -- Larsen, Kristopher -- McClintock, William E -- Stewart, A Ian F -- Hallett, Janet Tew -- Shemansky, Donald E -- Ajello, Joseph M -- Hansen, Candice J -- Hendrix, Amanda R -- West, Robert A -- Keller, H Uwe -- Korth, Axel -- Pryor, Wayne R -- Reulke, Ralf -- Yung, Yuk L -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1251-5. Epub 2004 Dec 16.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉University of Colorado, Laboratory for Atmospheric and Space Physics, 234 Innovation Drive, Boulder, CO 80303-7814, USA. larry.esposito@lasp.colorado.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15604361" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; *Hydrogen ; *Ice ; *Oxygen ; *Saturn ; Spacecraft ; Spectrum Analysis ; Ultraviolet Rays ; 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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  • 2
    Publication Date: 2006-03-11
    Description: The Cassini spacecraft flew close to Saturn's small moon Enceladus three times in 2005. Cassini's UltraViolet Imaging Spectrograph observed stellar occultations on two flybys and confirmed the existence, composition, and regionally confined nature of a water vapor plume in the south polar region of Enceladus. This plume provides an adequate amount of water to resupply losses from Saturn's E ring and to be the dominant source of the neutral OH and atomic oxygen that fill the Saturnian system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hansen, Candice J -- Esposito, L -- Stewart, A I F -- Colwell, J -- Hendrix, A -- Pryor, W -- Shemansky, D -- West, R -- New York, N.Y. -- Science. 2006 Mar 10;311(5766):1422-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA. Candice.j.Hansen@jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16527971" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment/chemistry ; Gases ; *Saturn ; Spacecraft ; Spectrophotometry, Ultraviolet ; 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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  • 3
    Publication Date: 2007-09-22
    Description: Water has supposedly marked the surface of Mars and produced characteristic landforms. To understand the history of water on Mars, we take a close look at key locations with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter, reaching fine spatial scales of 25 to 32 centimeters per pixel. Boulders ranging up to approximately 2 meters in diameter are ubiquitous in the middle to high latitudes, which include deposits previously interpreted as finegrained ocean sediments or dusty snow. Bright gully deposits identify six locations with very recent activity, but these lie on steep (20 degrees to 35 degrees) slopes where dry mass wasting could occur. Thus, we cannot confirm the reality of ancient oceans or water in active gullies but do see evidence of fluvial modification of geologically recent mid-latitude gullies and equatorial impact craters.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McEwen, A S -- Hansen, C J -- Delamere, W A -- Eliason, E M -- Herkenhoff, K E -- Keszthelyi, L -- Gulick, V C -- Kirk, R L -- Mellon, M T -- Grant, J A -- Thomas, N -- Weitz, C M -- Squyres, S W -- Bridges, N T -- Murchie, S L -- Seelos, F -- Seelos, K -- Okubo, C H -- Milazzo, M P -- Tornabene, L L -- Jaeger, W L -- Byrne, S -- Russell, P S -- Griffes, J L -- Martinez-Alonso, S -- Davatzes, A -- Chuang, F C -- Thomson, B J -- Fishbaugh, K E -- Dundas, C M -- Kolb, K J -- Banks, M E -- Wray, J J -- New York, N.Y. -- Science. 2007 Sep 21;317(5845):1706-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. mcewen@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17885125" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geological Phenomena ; Geology ; *Mars ; *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: 2011-02-05
    Description: Despite radically different environmental conditions, terrestrial and martian dunes bear a strong resemblance, indicating that the basic processes of saltation and grainfall (sand avalanching down the dune slipface) operate on both worlds. Here, we show that martian dunes are subject to an additional modification process not found on Earth: springtime sublimation of Mars' CO(2) seasonal polar caps. Numerous dunes in Mars' north polar region have experienced morphological changes within a Mars year, detected in images acquired by the High-Resolution Imaging Science Experiment on the Mars Reconnaissance Orbiter. Dunes show new alcoves, gullies, and dune apron extension. This is followed by remobilization of the fresh deposits by the wind, forming ripples and erasing gullies. The widespread nature of these rapid changes, and the pristine appearance of most dunes in the area, implicates active sand transport in the vast polar erg in Mars' current climate.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hansen, C J -- Bourke, M -- Bridges, N T -- Byrne, S -- Colon, C -- Diniega, S -- Dundas, C -- Herkenhoff, K -- McEwen, A -- Mellon, M -- Portyankina, G -- Thomas, N -- New York, N.Y. -- Science. 2011 Feb 4;331(6017):575-8. doi: 10.1126/science.1197636.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Science Institute, Tucson, AZ 85719, USA. cjhansen@psi.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21292976" target="_blank"〉PubMed〈/a〉
    Keywords: *Carbon Dioxide ; Dry Ice ; Extraterrestrial Environment ; *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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