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  • 1
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    Investigating the Stratigraphy of Mare Imbrium Flow Emplacement with Earth-Based Radar (2016)
    Wiley
    Details
    Publication Date: 2016-07-31
    Description: The lunar maria are the product of extensive basaltic volcanism that flooded widespread portions of the Moon's surface. Constraining mare volcanic history therefore provides a window into the endogenic processes responsible for shaping the Moon. Due to the low magma viscosity and the associated thin nature of lava units, the majority of mare surface structures are masked and subdued by impact regolith. Subtle individual mare flow morphologies, coupled with spatial limitations in the use of crater size distributions to distinguish surface units close in age, restricts our understanding of mare stratigraphy. Earth-based 70-cm wavelength (P-band) radar can reveal features beneath the regolith and highlight very subtle changes in the ilmenite content of the flows, providing a unique means to map mare units. Here we map volcanic units in Mare Imbrium using high-resolution (200 m/pixel), Earth-based P-band data. Situated within the heat-producing KREEP terrane, Mare Imbrium experienced some of the most long-lived (and recent) lunar volcanism, and its surface exhibits a significant diversity of basaltic chemistry. Our investigation identifies at least four distinct stages of volcanic activity, originating from multiple sources within Imbrium. The most recent of these stages comprises extensive, yet relatively thin volcanic flow units that left remnant kipukas of older mare material distributed across much of the basin. From a future mission perspective, it may be possible to collect samples expressing a wide range in age from small areas of Mare Imbrium. Our map also places important constraints on the interpretation of the Chang'E-3 Lunar Penetrating Radar measurements.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Radar evidence for liquid surfaces on Titan (2003)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2003-10-04
    Description: Arecibo radar observations of Titan at 13-centimeter wavelength indicate that most of the echo power is in a diffusely scattered component but that a small specular component is present for about 75% of the subearth locations observed. These specular echoes have properties consistent with those expected for areas of liquid hydrocarbons. Knowledge of the areal extent and depth of any deposits of liquid hydrocarbons could strongly constrain the history of Titan's atmosphere and surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Campbell, Donald B -- Black, Gregory J -- Carter, Lynn M -- Ostro, Steven J -- New York, N.Y. -- Science. 2003 Oct 17;302(5644):431-4. Epub 2003 Oct 2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Astronomy and Ionosphere Center and Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. campbell@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/14526087" target="_blank"〉PubMed〈/a〉
    Keywords: Astronomical Phenomena ; Astronomy ; Atmosphere ; Extraterrestrial Environment ; *Hydrocarbons ; Ice ; Radar ; *Saturn ; 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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  • 3
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    Radar observations of asteroid 216 kleopatra (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-05-08
    Description: Radar observations of the main-belt, M-class asteroid 216 Kleopatra reveal a dumbbell-shaped object with overall dimensions of 217 kilometers by 94 kilometers by 81 kilometers (+/-25%). The asteroid's surface properties are consistent with a regolith having a metallic composition and a porosity comparable to that of lunar soil. Kleopatra's shape is probably the outcome of an exotic sequence of collisional events, and much of its interior may have an unconsolidated rubble-pile structure.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro -- Hudson -- Nolan -- Margot -- Scheeres -- Campbell -- Magri -- Giorgini -- Yeomans -- New York, N.Y. -- Science. 2000 May 5;288(5467):836-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA. School of Electrical Engineering and Computer Science, Washington State University, Pullman, WA 99164-2752, USA. Arecibo Observatory, HC3 Box.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10797000" 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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  • 4
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    Topography of the lunar poles from radar interferometry: a survey of cold trap locations (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-06-05
    Description: Detailed topographic maps of the lunar poles have been obtained by Earth-based radar interferometry with the 3.5-centimeter wavelength Goldstone Solar System Radar. The interferometer provided maps 300 kilometers by 1000 kilometers of both polar regions at 150-meter spatial resolution and 50-meter height resolution. Using ray tracing, these digital elevation models were used to locate regions that are in permanent shadow from solar illumination and may harbor ice deposits. Estimates of the total extent of shadowed areas poleward of 87.5 degrees latitude are 1030 and 2550 square kilometers for the north and south poles, respectively.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Margot, J L -- Campbell, D B -- Jurgens, R F -- Slade, M A -- New York, N.Y. -- Science. 1999 Jun 4;284(5420):1658-60.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10356393" target="_blank"〉PubMed〈/a〉
    Keywords: *Ice ; Interferometry ; *Moon ; Radar ; 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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  • 5
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    Venus southern hemisphere: geologic character and age of terrains in the themis-alpha-lada region (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-01-11
    Description: Arecibo high-resolution radar images of the southern hemisphere of Venus extending to 78 degrees S show that the surface of the Themis-Alpha-Lada region is characterized by linear deformation zones with volcanoes and corona-like features and by regional volcanic deposits (primarily plains, small shields, and large edifices). Large-scale areal deformation is limited to the tessera of Alpha Regio. Lada Terra, in the southern high latitudes, contains several large coronae, in contrast to Ishtar Terra in the northern high latitudes. The density of craters of possible impact origin is somewhat lower than that observed in the Venera 15 and 16 coverage; these data extend to 43 percent of the areas of the surface of Venus with ages of less than about 1 billion years.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Campbell, D B -- Senske, D A -- Head, J W -- Hine, A A -- Fisher, P C -- New York, N.Y. -- Science. 1991 Jan 11;251(4990):180-3.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17836947" 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
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    Venus volcanism: initial analysis from magellan data (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    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
    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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  • 7
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    Magellan: electrical and physical properties of venus' surface (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    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〉
    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
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    Asteroid 1986 DA: Radar Evidence for a Metallic Composition (1991)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1991-06-07
    Description: Echoes from the near-Earth object 1986 DA show it to be significantly more reflective than other radar-detected asteroids. This result supports the hypothesis that 1986 DA is a piece of NiFe metal derived from the interior of a much larger object that melted, differentiated, cooled, and subsequently was disrupted in a catastrophic collision. This 2-kilometer asteroid, which appears smooth at centimeter to meter scales but extremely irregular at 10- to 100-meter scales, might be (or have been a part of the parent body of some iron meteorites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro, S J -- Campbell, D B -- Chandler, J F -- Hine, A A -- Hudson, R S -- Rosema, K D -- Shapiro, I I -- New York, N.Y. -- Science. 1991 Jun 7;252(5011):1399-404.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17772910" 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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  • 9
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    Impact craters on venus: initial analysis from magellan (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-04-12
    Description: Magellan radar images of 15 percent of the planet show 135 craters of probable impact origin. Craters more than 15 km across tend to contain central peaks, multiple central peaks, and peak rings. Many craters smaller than 15 km exhibit multiple floors or appear in clusters; these phenomena are attributed to atmospheric breakup of incoming meteoroids. Additionally, the atmosphere appears to have prevented the formation of primary impact craters smaller than about 3 km and produced a deficiency in the number of craters smaller than about 25 km across. Ejecta is found at greater distances than that predicted by simple ballistic emplacement, and the distal ends of some ejecta deposits are lobate. These characteristics may represent surface flows of material initially entrained in the atmosphere. Many craters are surrounded by zones of low radar albedo whose origin may have been deformation of the surface by the shock or pressure wave associated with the incoming meteoroid. Craters are absent from several large areas such as a 5 million square kilometer region around Sappho Patera, where the most likely explanation for the dearth of craters is volcanic resurfacing. There is apparently a spectrum of surface ages on Venus ranging approximately from 0 to 800 million years, and therefore Venus must be a geologically active planet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Phillips, R J -- Arvidson, R E -- Boyce, J M -- Campbell, D B -- Guest, J E -- Schaber, G G -- Soderblom, L A -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):288-97.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769276" 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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  • 10
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    Binary asteroids in the near-Earth object population (2002)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2002-04-16
    Description: Radar images of near-Earth asteroid 2000 DP107 show that it is composed of an approximately 800-meter-diameter primary and an approximately 300-meter-diameter secondary revolving around their common center of mass. The orbital period of 1.755 +/- 0.007 days and semimajor axis of 2620 +/- 160 meters constrain the total mass of the system to 4.6 +/- 0.5 x 10(11) kilograms and the bulk density of the primary to 1.7 +/- 1.1 grams per cubic centimeter. This system and other binary near-Earth asteroids have spheroidal primaries spinning near the breakup point for strengthless bodies, suggesting that the binaries formed by spin-up and fission, probably as a result of tidal disruption during close planetary encounters. About 16% of near-Earth asteroids larger than 200 meters in diameter may be binary systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Margot, J L -- Nolan, M C -- Benner, L A M -- Ostro, S J -- Jurgens, R F -- Giorgini, J D -- Slade, M A -- Campbell, D B -- New York, N.Y. -- Science. 2002 May 24;296(5572):1445-8. Epub 2002 Apr 11.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉California Institute of Technology, MC 150-21, Pasadena, CA 91125, USA. margot@gps.caltech.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11951001" 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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