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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
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  • 2
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    Estimating the mass of asteroid 433 eros during the NEAR spacecraft flyby (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-07-27
    Description: The Near Earth Asteroid Rendezvous (NEAR) spacecraft flew within 3830 kilometers of asteroid 433 Eros on 23 December 1998. The gravitational perturbation on NEAR was evident in the spacecraft tracking data. Ground-based Doppler and range tracking of the spacecraft as well as spacecraft images of the asteroid's center of figure and surface features were used to determine the mass and rotation pole of Eros. The mass of Eros is (7.2 +/- 1.8) x 10(18) grams and, coupled with a volume estimate provided by the NEAR imaging team, this mass suggests a bulk density of 2.5 +/- 0.8 grams per cubic centimeter. The rotation pole position is 15.6 (+/-3.7) degrees in right ascension and 16.4 (+/-1.8) degrees in declination, which is consistent with ground-based and NEAR imaging team observations.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Yeomans -- Antreasian -- Cheng -- Dunham -- Farquhar -- Gaskell -- Giorgini -- Helfrich -- Konopliv -- McAdams -- Miller -- Owen Jr -- Thomas -- Veverka -- Williams -- New York, N.Y. -- Science. 1999 Jul 23;285(5427):560-1.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Navigation and Flight Mechanics Section at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. Cornell University, Ithaca, NY.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10417380" target="_blank"〉PubMed〈/a〉
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  • 3
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    Imaging of small-scale features on 433 Eros from NEAR: evidence for a complex regolith (2001)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2001-04-21
    Description: On 25 October 2000, the Near Earth Asteroid Rendevous (NEAR)-Shoemaker spacecraft executed a low-altitude flyover of asteroid 433 Eros, making it possible to image the surface at a resolution of about 1 meter per pixel. The images reveal an evolved surface distinguished by an abundance of ejecta blocks, a dearth of small craters, and smooth material infilling some topographic lows. The subdued appearance of craters of different diameters and the variety of blocks and different degrees of their burial suggest that ejecta from several impact events blanketed the region imaged at closest approach and led to the building up of a substantial and complex regolith consisting of fine materials and abundant meter-sized blocks.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Veverka, J -- Thomas, P C -- Robinson, M -- Murchie, S -- Chapman, C -- Bell, M -- Harch, A -- Merline, W J -- Bell , J F 3rd -- Bussey, B -- Carcich, B -- Cheng, A -- Clark, B -- Domingue, D -- Dunham, D -- Farquhar, R -- Gaffey, M J -- Hawkins, E -- Izenberg, N -- Joseph, J -- Kirk, R -- Li, H -- Lucey, P -- Malin, M -- McFadden, L -- Miller, J K -- Owen , W M Jr -- Peterson, C -- Prockter, L -- Warren, J -- Wellnitz, D -- Williams, B G -- Yeomans, D K -- New York, N.Y. -- Science. 2001 Apr 20;292(5516):484-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉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/11313490" target="_blank"〉PubMed〈/a〉
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  • 4
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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〉
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  • 5
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    Radio science results during the NEAR-shoemaker spacecraft rendezvous with eros (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-09-23
    Description: We determined the mass of asteroid 433 Eros, its lower order gravitational harmonics, and rotation state, using ground-based Doppler and range tracking of the Near Earth Asteroid Rendezvous (NEAR)-Shoemaker spacecraft and images of the asteroid's surface landmarks. The mass of Eros is (6.687 +/- 0.003) x 10(18) grams, which, coupled with our volume estimate, implies a bulk density of 2. 67 +/- 0.03 grams per cubic centimeter. The asteroid appears to have a uniform density distribution. The right ascension and declination of the rotation pole are 11.37 +/- 0.05 and 17.22 +/- 0.05 degrees, respectively, and at least over the short term, the rotation state of Eros is stable with no measurable free precession of the spin pole. Escape velocities on the surface vary from 3.1 to 17.2 meters per second. The dynamical environment of Eros suggests that it is covered with regolith and that one might expect material transport toward the deepest potential wells in the saddle and 5.5-kilometer crater regions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Yeomans -- Antreasian -- Barriot -- Chesley -- Dunham -- Farquhar -- Giorgini -- Helfrich -- Konopliv -- McAdams -- Miller -- Owen Jr -- Scheeres -- Thomas -- Veverka -- Williams -- New York, N.Y. -- Science. 2000 Sep 22;289(5487):2085-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Navigation and Mission Design Section, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. Department of Terrestrial and Planetary Geodesy, Centre National d'Etudes Spatiales, Toulouse, France. Applied.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11000104" target="_blank"〉PubMed〈/a〉
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  • 6
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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〉
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  • 7
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    Detection of soft X-rays and a sensitive search for noble gases in comet Hale-Bopp (1997)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1997-09-05
    Description: An image of comet Hale-Bopp (C/1995 O1) in soft x-rays reveals a central emission offset from the nucleus, as well as an extended emission feature that does not correlate with the dust jets seen at optical wavelengths. Neon was found to be depleted in the cometary ice by more than a factor of 25 relative to solar abundance, which suggests that ices in Hale-Bopp formed at (or later experienced) temperatures higher than 25 kelvin. A helium line emission at a wavelength of 584 angstroms was detected and may be attributable to charge transfer of solar wind alpha particles in the cometary coma. Ionized oxygen and another helium line contribute to an emission observed at 538 angstroms.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krasnopolsky, V A -- Mumma, M J -- Abbott, M -- Flynn, B C -- Meech, K J -- Yeomans, D K -- Feldman, P D -- Cosmovici, C B -- New York, N.Y. -- Science. 1997 Sep 5;277(5331):1488-91.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Catholic University of America, Washington, DC 20064, USA. ys2VK@lepvax.gsfc.nasa.gov 20771, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9278508" target="_blank"〉PubMed〈/a〉
    Keywords: Cosmic Dust ; Helium/*analysis ; Ice ; *Meteoroids ; Neon/*analysis ; Oxygen/*analysis ; Temperature ; X-Rays
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  • 8
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    Radar Image of Asteroid 1989 PB (1990)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1990-06-22
    Description: Radar observations of the near-Earth asteroid 1989 PB, made shortly after its optical discovery, yield a sequence of delay-Doppler images that reveal it to consist of two distinct lobes that appear to be in contact. It seems likely that the two lobes once were separate and that they collided to produce the current "contact-binary" configuration.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ostro, S J -- Chandler, J F -- Hine, A A -- Rosema, K D -- Shapiro, I I -- Yeomans, D K -- New York, N.Y. -- Science. 1990 Jun 22;248(4962):1523-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17818312" target="_blank"〉PubMed〈/a〉
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  • 9
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    Radar detection of phobos (1989)
    American Association for the Advancement of Science (AAAS)
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    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〉
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  • 10
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    EPOXI at comet Hartley 2 (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-06-18
    Description: Understanding how comets work--what drives their activity--is crucial to the use of comets in studying the early solar system. EPOXI (Extrasolar Planet Observation and Deep Impact Extended Investigation) flew past comet 103P/Hartley 2, one with an unusually small but very active nucleus, taking both images and spectra. Unlike large, relatively inactive nuclei, this nucleus is outgassing primarily because of CO(2), which drags chunks of ice out of the nucleus. It also shows substantial differences in the relative abundance of volatiles from various parts of the nucleus.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉A'Hearn, Michael F -- Belton, Michael J S -- Delamere, W Alan -- Feaga, Lori M -- Hampton, Donald -- Kissel, Jochen -- Klaasen, Kenneth P -- McFadden, Lucy A -- Meech, Karen J -- Melosh, H Jay -- Schultz, Peter H -- Sunshine, Jessica M -- Thomas, Peter C -- Veverka, Joseph -- Wellnitz, Dennis D -- Yeomans, Donald K -- Besse, Sebastien -- Bodewits, Dennis -- Bowling, Timothy J -- Carcich, Brian T -- Collins, Steven M -- Farnham, Tony L -- Groussin, Olivier -- Hermalyn, Brendan -- Kelley, Michael S -- Li, Jian-Yang -- Lindler, Don J -- Lisse, Carey M -- McLaughlin, Stephanie A -- Merlin, Frederic -- Protopapa, Silvia -- Richardson, James E -- Williams, Jade L -- New York, N.Y. -- Science. 2011 Jun 17;332(6036):1396-400. doi: 10.1126/science.1204054.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Maryland, College Park, MD 20742-2421 USA. ma@astro.umd.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21680835" target="_blank"〉PubMed〈/a〉
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