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  • 1
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    In:  Eos, Trans., Am. Geophys. Un., Warszawa, Polish Geothermal Association, vol. 84, no. 45, pp. 485, 491, pp. B05406, (ISSN: 1340-4202)
    Publication Date: 2003
    Keywords: Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Geodesy ; Global Positioning System ; InSAR ; Strain ; Stress
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  • 2
    Publication Date: 1991-04-12
    Description: Initial Magellan observations reveal a planet with high dielectric constant materials exposed preferentially in elevated regions with high slopes, ejecta deposits extending up to 1000 kilometers to the west of several impact craters, windblown deposits and features in areas where there are both obstacles and a source of particulate material, and evidence for slow, steady degradation by atmosphere-surface interactions and mass movements.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Arvidson, R E -- Baker, V R -- Elachi, C -- Saunders, R S -- Wood, J A -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):270-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769274" target="_blank"〉PubMed〈/a〉
    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: 1991-04-12
    Description: Magellan images confirm that volcanism is widespread and has been fimdamentally important in the formation and evolution of the crust of Venus. High-resolution imaging data reveal evidence for intrusion (dike formation and cryptodomes) and extrusion (a wide range of lava flows). Also observed are thousands of small shield volcanoes, larger edifices up to several hundred kilometers in diameter, massive outpourings of lavas, and local pyroclastic deposits. Although most features are consistent with basaltic compositions, a number of large pancake-like domes are morphologically similar to rhyolite-dacite domes on Earth. Flows and sinuous channels with lengths of many hundreds of kilometers suggest that extremely high effusion rates or very fluid magmas (perhaps komatiites) may be present. Volcanism is evident in various tectonic settings (coronae, linear extensional and compressional zones, mountain belts, upland rises, highland plateaus, and tesserae). Volcanic resurfacing rates appear to be low (less than 2 Km(3)/yr) but the significance of dike formation and intrusions, and the mode of crustal formation and loss remain to be established.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Head, J W -- Campbell, D B -- Elachi, C -- Guest, J E -- McKenzie, D P -- Saunders, R S -- Schaber, G G -- Schubert, G -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):276-88.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769275" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
    Publication Date: 1991-04-12
    Description: Magellan probes Venus' surface by 12.6-cm-wavelength vertical and oblique radar scattering and measures microwave thermal emission. Emissivity and root-meansquare slope maps between 330 degrees and 30 degrees E and 90 degrees N and 80 degrees S are dissimilar, although some local features are exceptions. Inferred surface emissivities typically are approximately 0.85, but vary from approximately 0.35 at Maxwell to approximately 0.95 northeast of Gula Mons and other locations. Lowest emissivities appear in topographically high areas; this relation suggests that a phase change or differences in chemical weathering occur at about 6055-kilometer radius. Initial results indicate that there are significant variations in the surface scattering function.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Tyler, G L -- Ford, P G -- Campbell, D B -- Elachi, C -- Pettengill, G H -- Simpson, R A -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):265-70.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769273" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
    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
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 6
    Publication Date: 2005-05-14
    Description: The Cassini Titan Radar Mapper imaged about 1% of Titan's surface at a resolution of approximately 0.5 kilometer, and larger areas of the globe in lower resolution modes. The images reveal a complex surface, with areas of low relief and a variety of geologic features suggestive of dome-like volcanic constructs, flows, and sinuous channels. The surface appears to be young, with few impact craters. Scattering and dielectric properties are consistent with porous ice or organics. Dark patches in the radar images show high brightness temperatures and high emissivity and are consistent with frozen hydrocarbons.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Elachi, C -- Wall, S -- Allison, M -- Anderson, Y -- Boehmer, R -- Callahan, P -- Encrenaz, P -- Flamini, E -- Franceschetti, G -- Gim, Y -- Hamilton, G -- Hensley, S -- Janssen, M -- Johnson, W -- Kelleher, K -- Kirk, R -- Lopes, R -- Lorenz, R -- Lunine, J -- Muhleman, D -- Ostro, S -- Paganelli, F -- Picardi, G -- Posa, F -- Roth, L -- Seu, R -- Shaffer, S -- Soderblom, L -- Stiles, B -- Stofan, E -- Vetrella, S -- West, R -- Wood, C -- Wye, L -- Zebker, H -- New York, N.Y. -- Science. 2005 May 13;308(5724):970-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15890871" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; Hydrocarbons ; Ice ; Organic Chemicals ; Radar ; *Saturn ; *Spacecraft ; Temperature ; Volcanic Eruptions
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    Electronic ISSN: 1095-9203
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  • 7
    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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  • 8
    Publication Date: 2015-08-01
    Description: The Philae lander provides a unique opportunity to investigate the internal structure of a comet nucleus, providing information about its formation and evolution in the early solar system. We present Comet Nucleus Sounding Experiment by Radiowave Transmission (CONSERT) measurements of the interior of Comet 67P/Churyumov-Gerasimenko. From the propagation time and form of the signals, the upper part of the "head" of 67P is fairly homogeneous on a spatial scale of tens of meters. CONSERT also reduced the size of the uncertainty of Philae's final landing site down to approximately 21 by 34 square meters. The average permittivity is about 1.27, suggesting that this region has a volumetric dust/ice ratio of 0.4 to 2.6 and a porosity of 75 to 85%. The dust component may be comparable to that of carbonaceous chondrites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kofman, Wlodek -- Herique, Alain -- Barbin, Yves -- Barriot, Jean-Pierre -- Ciarletti, Valerie -- Clifford, Stephen -- Edenhofer, Peter -- Elachi, Charles -- Eyraud, Christelle -- Goutail, Jean-Pierre -- Heggy, Essam -- Jorda, Laurent -- Lasue, Jeremie -- Levasseur-Regourd, Anny-Chantal -- Nielsen, Erling -- Pasquero, Pierre -- Preusker, Frank -- Puget, Pascal -- Plettemeier, Dirk -- Rogez, Yves -- Sierks, Holger -- Statz, Christoph -- Svedhem, Hakan -- Williams, Iwan -- Zine, Sonia -- Van Zyl, Jakob -- New York, N.Y. -- Science. 2015 Jul 31;349(6247):aab0639. doi: 10.1126/science.aab0639.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Universite Grenoble Alpes, IPAG, F-38000 Grenoble, France (2) Centre National de la Recherche Scientifique (CNRS), Institut de Planetologie et d'Astrophysique de Grenoble (IPAG), F-38000 Grenoble, France. ; MIO, UM 110, CNRS-Institut National des Sciences de l'Univers (INSU), Universite de Toulon, Aix-Marseille Universite, IRD 83957 La Garde, France. ; Geodesy Observatory of Tahiti BP6570, 98702 Faa'a, Tahiti. ; Universite de Versailles Saint-Quentin-en-Yvelines (UVSQ) (UPSay); Universite Pierre et Marie Curie (UPMC) (Sorbonne Univ.); CNRS/INSU; Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS)-Institut Pierre-Simon Laplace (IPSL), 11 Boulevard d'Alembert, 78280 Guyancourt, France. ; Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058, USA. ; Ruhr-University of Bochum, Faculty of Electrical Engineering and Information Technology, 44780 Bochum, Germany. ; Jet Propulsion Laboratory, 4800 Oak Grove Drive, MS 300-243E, Pasadena, CA 91109, USA. ; Aix-Marseille Universite, CNRS, Centrale Marseille, Institut Fresnel UMR 7249, 13013 Marseille, France. ; Jet Propulsion Laboratory, 4800 Oak Grove Drive, MS 300-243E, Pasadena, CA 91109, USA. University of Southern California, Ming Hsieh Department of Electrical Engineering, Viterbi School of Engineering, Los Angeles, CA 90089, USA. ; Laboratoire d'Astrophysique de Marseille Pole de l'Etoile Site de Chateau-Gombert 38, Rue Frederic Joliot-Curie 13388 Marseille, France. ; Universite de Toulouse; UPS-OMP; IRAP; (2) CNRS; IRAP; 9 Avenue Colonel Roche, BP 44 346, F-31028 Toulouse Cedex 4, Toulouse, France. ; UPMC (Sorbonne Univ.); UVSQ (UPSay); CNRS/INSU; LATMOS-IPSL, BC 102, 4 place Jussieu, 75005 Paris, France. ; Max-Planck-Institut fur Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; German Aerospace Center (DLR) Rutherfordstrasse 2 12489 Berlin, Germany. ; Technische Universitaet Dresden Helmholtzstrasse 10 D-01069 Dresden, Germany. ; European Space Agency (ESA)/European Space Research and Technology Centre (ESTEC) Noordwijk, Netherlands. ; Queen Mary University of London, Mile End Road, London E1 4NS, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26228153" target="_blank"〉PubMed〈/a〉
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  • 9
    Publication Date: 1982-12-03
    Description: The shuttle imaging radar (SIR-A) acquired images of a variety of the earth's geologic areas covering about 10 million square kilometers. Structural and geomorphic features such as faults, folds, outcrops, and dunes are clearly visible in both tropical and arid regions. The combination of SIR-A and Seasat images provides additional information about the surface physical properties: topography and roughness. Ocean features were also observed, including large internal waves in the Andaman Sea.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Elachi, C -- Brown, W E -- Cimino, J B -- Dixon, T -- Evans, D L -- Ford, J P -- Saunders, R S -- Breed, C -- Masursky, H -- McCauley, J F -- Schaber, G -- Dellwig, L -- England, A -- Macdonald, H -- Martin-Kaye, P -- Sabins, F -- New York, N.Y. -- Science. 1982 Dec 3;218(4576):996-1003.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17790588" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 1982-12-03
    Description: The shuttle imaging radar (SIR-A) carried on the space shuttle Columbia in November 1981 penetrated the extremely dry Selima Sand Sheet, dunes, and drift sand of the eastern Sahara, revealing previously unknown buried valleys, geologic structures, and possible Stone Age occupation sites. Radar responses from bedrock and gravel surfaces beneath windblown sand several centimeters to possibly meters thick delineate sand- and alluvium-filled valleys, some nearly as wide as the Nile Valley and perhaps as old as middle Tertiary. The now-vanished major river systems that carved these large valleys probably accomplished most of the erosional stripping of this extraordinarily flat, hyperarid region. Underfit and incised dry wadis, many superimposed on the large valleys, represent erosion by intermittent running water, probably during Quaternary pluvials. Stone Age artifacts associated with soils in the alluvium suggest that areas near the wadis may have been sites of early human occupation. The presence of old drainage networks beneath the sand sheet provides a geologic explanation for the locations of many playas and present-day oases which have been centers of episodic human habitation. Radar penetration of dry sand and soils varies with the wavelength of the incident signals (24 centimeters for the SIR-A system), incidence angle, and the electrical properties of the materials, which are largely determined by moisture content. The calculated depth of radar penetration of dry sand and granules, based on laboratory measurements of the electrical properties of samples from the Selima Sand Sheet, is at least 5 meters. Recent (September 1982) field studies in Egypt verified SIR-A signal penetration depths of at least 1 meter in the Selima Sand Sheet and in drift sand and 2 or more meters in sand dunes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McCauley, J F -- Schaber, G G -- Breed, C S -- Grolier, M J -- Haynes, C V -- Issawi, B -- Elachi, C -- Blom, R -- New York, N.Y. -- Science. 1982 Dec 3;218(4576):1004-20.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17790589" target="_blank"〉PubMed〈/a〉
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