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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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    Asteroid 1950 DA's encounter with Earth in 2880: physical limits of collision probability prediction (2002)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2002-04-06
    Description: Integration of the orbit of asteroid (29075) 1950 DA, which is based on radar and optical measurements spanning 51 years, reveals a 20-minute interval in March 2880 when there could be a nonnegligible probability of the 1-kilometer object colliding with Earth. Trajectory knowledge remains accurate until then because of extensive astrometric data, an inclined orbit geometry that reduces in-plane perturbations, and an orbit uncertainty space modulated by gravitational resonance. The approach distance uncertainty in 2880 is determined primarily by uncertainty in the accelerations arising from thermal re-radiation of solar energy absorbed by the asteroid. Those accelerations depend on the spin axis, composition, and surface properties of the asteroid, so that refining the collision probability may require direct inspection by a spacecraft.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Giorgini, J D -- Ostro, S J -- Benner, L A M -- Chodas, P W -- Chesley, S R -- Hudson, R S -- Nolan, M C -- Klemola, A R -- Standish, E M -- Jurgens, R F -- Rose, R -- Chamberlin, A B -- Yeomans, D K -- Margot, J L -- New York, N.Y. -- Science. 2002 Apr 5;296(5565):132-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA. Jon.Giorgini@jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11935024" 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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  • 3
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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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  • 4
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    Radar detection of phobos (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-03-24
    Description: Radar echoes from the martian satellite Phobos provide information about that object's surface properties at scales near the 3.5-cm observing wavelength. Phobos appears less rough than the moon at centimeter-to-decimeter scales. The uppermost few decimeters of the satellite's regolith have a mean bulk density within 20% of 2.0 g cm(-3). The radar signature of Phobos (albedo, polarization ratio, and echo spectral shape) differs from signatures measured for small, Earth-approaching objects, but resembles those of large (〉/=100-km), C-class, mainbelt asteroids.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro, S J -- Jurgens, R F -- Yeomans, D K -- Standish, E M -- Greiner, W -- New York, N.Y. -- Science. 1989 Mar 24;243(4898):1584-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17847261" 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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  • 5
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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〉
    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
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    Radar detection of the nucleus and coma of comet hyakutake (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    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〉
    Print ISSN: 0036-8075
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  • 7
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    Binary asteroids in the near-Earth object population (2002)
    American Association for the Advancement of Science (AAAS)
    Details
    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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  • 8
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    Dynamical configuration of binary near-Earth asteroid (66391) 1999 KW4 (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-10-14
    Description: Dynamical simulations of the coupled rotational and orbital dynamics of binary near-Earth asteroid 66391 (1999 KW4) suggest that it is excited as a result of perturbations from the Sun during perihelion passages. Excitation of the mutual orbit will stimulate complex fluctuations in the orbit and rotation of both components, inducing the attitude of the smaller component to have large variation within some orbits and to hardly vary within others. The primary's proximity to its rotational stability limit suggests an origin from spin-up and disruption of a loosely bound precursor within the past million years.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Scheeres, D J -- Fahnestock, E G -- Ostro, S J -- Margot, J-L -- Benner, L A M -- Broschart, S B -- Bellerose, J -- Giorgini, J D -- Nolan, M C -- Magri, C -- Pravec, P -- Scheirich, P -- Rose, R -- Jurgens, R F -- De Jong, E M -- Suzuki, S -- New York, N.Y. -- Science. 2006 Nov 24;314(5803):1280-3. Epub 2006 Oct 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Aerospace Engineering, University of Michigan, 1320 Beal Avenue, Ann Arbor, MI 48109-2140, USA. scheeres@umich.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17038588" target="_blank"〉PubMed〈/a〉
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  • 9
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    Radar imaging of binary near-Earth asteroid (66391) 1999 KW4 (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-10-14
    Description: High-resolution radar images reveal near-Earth asteroid (66391) 1999 KW4 to be a binary system. The approximately 1.5-kilometer-diameter primary (Alpha) is an unconsolidated gravitational aggregate with a spin period approximately 2.8 hours, bulk density approximately 2 grams per cubic centimeter, porosity approximately 50%, and an oblate shape dominated by an equatorial ridge at the object's potential-energy minimum. The approximately 0.5-kilometer secondary (Beta) is elongated and probably is denser than Alpha. Its average orbit about Alpha is circular with a radius approximately 2.5 kilometers and period approximately 17.4 hours, and its average rotation is synchronous with the long axis pointed toward Alpha, but librational departures from that orientation are evident. Exotic physical and dynamical properties may be common among near-Earth binaries.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro, Steven J -- Margot, Jean-Luc -- Benner, Lance A M -- Giorgini, Jon D -- Scheeres, Daniel J -- Fahnestock, Eugene G -- Broschart, Stephen B -- Bellerose, Julie -- Nolan, Michael C -- Magri, Christopher -- Pravec, Petr -- Scheirich, Petr -- Rose, Randy -- Jurgens, Raymond F -- De Jong, Eric M -- Suzuki, Shigeru -- New York, N.Y. -- Science. 2006 Nov 24;314(5803):1276-80. Epub 2006 Oct 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA. ostro@reason.jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17038586" 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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