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  • 1
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    Radar and optical observations of asteroid 1998 KY26 (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-07-27
    Description: Observations of near-Earth asteroid 1998 KY26 shortly after its discovery reveal a slightly elongated spheroid with a diameter of about 30 meters, a composition analogous to carbonaceous chondritic meteorites, and a rotation period of 10.7 minutes, which is an order of magnitude shorter than that measured for any other solar system object. The rotation is too rapid for 1998 KY26 to consist of multiple components bound together just by their mutual gravitational attraction. This monolithic object probably is a fragment derived from cratering or collisional destruction of a much larger asteroid.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro -- Pravec -- Benner -- Hudson -- Sarounova -- Hicks -- Rabinowitz -- Scotti -- Tholen -- Wolf -- Jurgens -- Thomas -- Giorgini -- Chodas -- Yeomans -- Rose -- Frye -- Rosema -- Winkler -- Slade -- New York, N.Y. -- Science. 1999 Jul 23;285(5427):557-60.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA. Astronomical Institute, Academy of Sciences of the Czech Republic, CZ-25165 Ond&rbreve;ejov, Czech Republic. School of Electrical Engineering and.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10417379" 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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  • 2
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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
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  • 3
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    Radar reflectivity of titan (1990)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1990-05-25
    Description: The present understanding of the atmosphere and surface conditions on Saturn's largest moon, Titan, including the stability of methane, and an application of thermodynamics leads to a strong prediction of liquid hydrocarbons in an ethane-methane mixture on the surface. Such a surface would have nearly unique microwave reflection properties due to the low dielectric constant. Attempts were made to obtain reflections at a wavelength of 3.5 centimeters by means of a 70-meter antenna in California as the transmitter and the Very Large Array in New Mexico as the receiving instrument. Statistically significant echoes were obtained that show Titan is not covered with a deep, global ocean of ethane, as previously thought. The experiment yielded radar cross sections normalized by the Titan disk of 0.38 +/- 0.15, 0.78 +/- 0.15, and 0.25 +/- 0.15 on three consecutive nights during which the sub-Earth longitude on Titan moved 50 degrees. The result for the combined data for the entire experiment is 0.35 +/- 0.08. The cross sections are very high, most consistent with those of the Galilean satellites; no evidence of the putative liquid ethane was seen in the reflection data. A global ocean as shallow as about 200 meters would have exhibited reflectivities smaller by an order of magnitude, and below the detection limit of the experiment. The measured emissivity at similar wavelengths of about 0.9 is somewhat inconsistent with the high reflectivity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Muhleman, D O -- Grossman, A W -- Butler, B J -- Slade, M A -- New York, N.Y. -- Science. 1990 May 25;248(4958):975-80.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17745402" target="_blank"〉PubMed〈/a〉
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  • 4
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    Radar images of Mars (1991)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1991-09-27
    Description: Full disk images of Mars have been obtained with the use of the Very Large Array (VLA) to map the radar reflected flux density. The transmitter system was the 70-m antenna of the Deep Space Network at Goldstone, California. The surface of Mars was illuminated with continuous wave radiation at a wavelength of 3,5 cm. The reflected energy was mapped in individual 12-minute snapshots with the VLA in its largest configuration; fringe spacings as small as 67 km were obtained. The images reveal near-surface features including a region in the Tharsis volcano area, over 2000 km in east-west extent, that displayed no echo to the very low level of the radar system noise. The feature, called Stealth, is interpreted as a deposit of dust or ash with a density less than about 0.5 gram per cubic centimeter and free of rocks larger than 1 cm across. The deposit must be several meters thick and may be much deeper. The strongest reflecting geological feature was the south polar ice cap, which was reduced in size to the residual south polar ice cap at the season of observation. The cap image is interpreted as arising from nearly pure CO(2) or H(2)O ice with a small amount of martian dust (less than 2 percent by volume) and a depth greater than 2 to 5 m. Only one anomalous reflecting feature was identified outside of the Tharsis region, although the Elysium region was poorly sampled in this experiment and the north pole was not visible from Earth.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Muhleman, D O -- Butler, B J -- Grossman, A W -- Slade, M A -- New York, N.Y. -- Science. 1991 Sep 27;253(5027):1508-13.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17784090" target="_blank"〉PubMed〈/a〉
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  • 5
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    Mercury radar imaging: evidence for polar ice (1992)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1992-10-23
    Description: The first unambiguous full-disk radar mapping of Mercury at 3.5-centimeter wavelength, with the Goldstone 70-meter antenna transmitting and 26 antennas of the Very Large Array receiving, has provided evidence for the presence of polar ice. The radar experiments, conducted on 8 and 23 August 1991, were designed to image the half of Mercury not photographed by Mariner 10. The orbital geometry allowed viewing beyond the north pole of Mercury; a highly reflective region was clearly visible on the north pole during both experiments. This polar region has areas in which the circular polarization ratio (pt) was 1.0 to 1.4; values 〈 approximately 0.1 are typical for terrestrial planets. Such high values of have hitherto been observed in radar observations only from icy regions of Mars and icy outer planet satellites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Slade, M A -- Butler, B J -- Muhleman, D O -- New York, N.Y. -- Science. 1992 Oct 23;258(5082):635-40.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748898" target="_blank"〉PubMed〈/a〉
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  • 6
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    Large longitude libration of Mercury reveals a molten core (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2007-05-05
    Description: Observations of radar speckle patterns tied to the rotation of Mercury establish that the planet occupies a Cassini state with obliquity of 2.11 +/- 0.1 arc minutes. The measurements show that the planet exhibits librations in longitude that are forced at the 88-day orbital period, as predicted by theory. The large amplitude of the oscillations, 35.8 +/- 2 arc seconds, together with the Mariner 10 determination of the gravitational harmonic coefficient C22, indicates that the mantle of Mercury is decoupled from a core that is at least partially molten.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Margot, J L -- Peale, S J -- Jurgens, R F -- Slade, M A -- Holin, I V -- New York, N.Y. -- Science. 2007 May 4;316(5825):710-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Cornell University, 304 Space Sciences Building, Ithaca, NY 14853, USA. jlm@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17478713" target="_blank"〉PubMed〈/a〉
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  • 7
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    Radar detection of the nucleus and coma of comet hyakutake (1997)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1997-12-24
    Description: Radar observations of comet Hyakutake (C/1996 B2) made at the Goldstone Deep Space Communications Complex in California have detected echoes from the nucleus and from large grains in the inner coma. The nucleus of this bright comet was estimated to be only 2 to 3 kilometers in diameter. Models of the coma echo indicate backscatter from porous, centimeter-size grains ejected anisotropically at velocities of tens of meters per second. The radar observations suggest that a comet's activity may be a poor indicator of its size and provide evidence that large grains constitute an important component of the mass loss from a typical active comet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Harmon -- Ostro -- Benner -- Rosema -- Jurgens -- Winkler -- Yeomans -- Choate -- Cormier -- Giorgini -- Mitchell -- Chodas -- Rose -- Kelley -- Slade -- Thomas -- New York, N.Y. -- Science. 1997 Dec 12;278(5345):1921-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉J. K. Harmon, National Astronomy and Ionosphere Center, Arecibo Observatory, Post Office Box 995, Arecibo, PR 00614, USA. S. J. Ostro, L. A. M. Benner, K. D. Rosema, R. F. Jurgens, R. Winkler, D. K. Yeomans, D. Choate, R. Cormier, J. D. Giorg.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9395389" target="_blank"〉PubMed〈/a〉
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  • 8
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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〉
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  • 9
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    Radar mapping of mercury: full-disk images and polar anomalies (1992)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1992-10-23
    Description: A random-code technique has been used at Arecibo to obtain delay-Doppler radar images of the full disk of Mercury. Anomalously bright features were found at the north and south poles. The north polar feature is oblong (4 degrees by 8 degrees ) and offset from the pole. The smaller south polar feature is mostly confined to the floor of the crater Chao Meng-Fu. The polar locations and radar properties of these features indicate that they may be produced by volume scattering in ice. The images also reveal a variety of more subdued reflectivity features ranging in size from hundreds to thousands of kilometers; some of these appear to have an impact origin.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Harmon, J K -- Slade, M A -- New York, N.Y. -- Science. 1992 Oct 23;258(5082):640-3.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17748899" target="_blank"〉PubMed〈/a〉
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  • 10
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    Evidence for highly reflecting materials on the surface and subsurface of vensus (1988)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1988-05-20
    Description: Radar images at a 12.5-centimeter wavelength made with the Goldstone radar interferometer in 1980 and 1986, together with lunar radar images and recent Venera 15 and 16 data, indicate that material on the surface and subsurface of Venus has a Fresnel reflectivity in excess of 50 percent. Such high reflectivities have been reported on the surface in mountainous regions. Material of high reflectivity may also underlie lower reflectivity surficial materials of the plains regions, where it has been excavated by impact cratering in some areas.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jurgens, R F -- Slade, M A -- Saunders, R S -- New York, N.Y. -- Science. 1988 May 20;240(4855):1021-3.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17731715" target="_blank"〉PubMed〈/a〉
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