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  • 1
    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
    Publication Date: 2010-08-27
    Description: Pairs of asteroids sharing similar heliocentric orbits, but not bound together, were found recently. Backward integrations of their orbits indicated that they separated gently with low relative velocities, but did not provide additional insight into their formation mechanism. A previously hypothesized rotational fission process may explain their formation-critical predictions are that the mass ratios are less than about 0.2 and, as the mass ratio approaches this upper limit, the spin period of the larger body becomes long. Here we report photometric observations of a sample of asteroid pairs, revealing that the primaries of pairs with mass ratios much less than 0.2 rotate rapidly, near their critical fission frequency. As the mass ratio approaches 0.2, the primary period grows long. This occurs as the total energy of the system approaches zero, requiring the asteroid pair to extract an increasing fraction of energy from the primary's spin in order to escape. We do not find asteroid pairs with mass ratios larger than 0.2. Rotationally fissioned systems beyond this limit have insufficient energy to disrupt. We conclude that asteroid pairs are formed by the rotational fission of a parent asteroid into a proto-binary system, which subsequently disrupts under its own internal system dynamics soon after formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pravec, P -- Vokrouhlicky, D -- Polishook, D -- Scheeres, D J -- Harris, A W -- Galad, A -- Vaduvescu, O -- Pozo, F -- Barr, A -- Longa, P -- Vachier, F -- Colas, F -- Pray, D P -- Pollock, J -- Reichart, D -- Ivarsen, K -- Haislip, J -- Lacluyze, A -- Kusnirak, P -- Henych, T -- Marchis, F -- Macomber, B -- Jacobson, S A -- Krugly, Yu N -- Sergeev, A V -- Leroy, A -- England -- Nature. 2010 Aug 26;466(7310):1085-8. doi: 10.1038/nature09315.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomical Institute AS CR, Fricova 1, CZ-25165 Ondrejov, Czech Republic. ppravec@asu.cas.cz〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20740010" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 3
    Publication Date: 2009-03-28
    Description: In the absence of a firm link between individual meteorites and their asteroidal parent bodies, asteroids are typically characterized only by their light reflection properties, and grouped accordingly into classes. On 6 October 2008, a small asteroid was discovered with a flat reflectance spectrum in the 554-995 nm wavelength range, and designated 2008 TC(3) (refs 4-6). It subsequently hit the Earth. Because it exploded at 37 km altitude, no macroscopic fragments were expected to survive. Here we report that a dedicated search along the approach trajectory recovered 47 meteorites, fragments of a single body named Almahata Sitta, with a total mass of 3.95 kg. Analysis of one of these meteorites shows it to be an achondrite, a polymict ureilite, anomalous in its class: ultra-fine-grained and porous, with large carbonaceous grains. The combined asteroid and meteorite reflectance spectra identify the asteroid as F class, now firmly linked to dark carbon-rich anomalous ureilites, a material so fragile it was not previously represented in meteorite collections.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jenniskens, P -- Shaddad, M H -- Numan, D -- Elsir, S -- Kudoda, A M -- Zolensky, M E -- Le, L -- Robinson, G A -- Friedrich, J M -- Rumble, D -- Steele, A -- Chesley, S R -- Fitzsimmons, A -- Duddy, S -- Hsieh, H H -- Ramsay, G -- Brown, P G -- Edwards, W N -- Tagliaferri, E -- Boslough, M B -- Spalding, R E -- Dantowitz, R -- Kozubal, M -- Pravec, P -- Borovicka, J -- Charvat, Z -- Vaubaillon, J -- Kuiper, J -- Albers, J -- Bishop, J L -- Mancinelli, R L -- Sandford, S A -- Milam, S N -- Nuevo, M -- Worden, S P -- England -- Nature. 2009 Mar 26;458(7237):485-8. doi: 10.1038/nature07920.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉SETI Institute, Carl Sagan Center, 515 North Whisman Road, Mountain View, California 94043, USA. Petrus.M.Jenniskens@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19325630" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 4
    Publication Date: 2007-03-10
    Description: Radar and optical observations reveal that the continuous increase in the spin rate of near-Earth asteroid (54509) 2000 PH5 can be attributed to the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, a torque due to sunlight. The change in spin rate is in reasonable agreement with theoretical predictions for the YORP acceleration of a body with the radar-determined size, shape, and spin state of 2000 PH5. The detection of asteroid spin-up supports the YORP effect as an explanation for the anomalous distribution of spin rates for asteroids under 10 kilometers in diameter and as a binary formation mechanism.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Taylor, Patrick A -- Margot, Jean-Luc -- Vokrouhlicky, David -- Scheeres, Daniel J -- Pravec, Petr -- Lowry, Stephen C -- Fitzsimmons, Alan -- Nolan, Michael C -- Ostro, Steven J -- Benner, Lance A M -- Giorgini, Jon D -- Magri, Christopher -- New York, N.Y. -- Science. 2007 Apr 13;316(5822):274-7. Epub 2007 Mar 8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Cornell University, Ithaca, NY 14853-6801, USA. ptaylor@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17347415" 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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  • 5
    Publication Date: 2007-03-10
    Description: The Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect is believed to alter the spin states of small bodies in the solar system. However, evidence for the effect has so far been indirect. We report precise optical photometric observations of a small near-Earth asteroid, (54509) 2000 PH5, acquired over 4 years. We found that the asteroid has been continuously increasing its rotation rate omega over this period by domega/dt = 2.0 (+/-0.2) x 10(-4) degrees per day squared. We simulated the asteroid's close Earth approaches from 2001 to 2005, showing that gravitational torques cannot explain the observed spin rate increase. Dynamical simulations suggest that 2000 PH5 may reach a rotation period of approximately 20 seconds toward the end of its expected lifetime.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lowry, Stephen C -- Fitzsimmons, Alan -- Pravec, Petr -- Vokrouhlicky, David -- Boehnhardt, Hermann -- Taylor, Patrick A -- Margot, Jean-Luc -- Galad, Adrian -- Irwin, Mike -- Irwin, Jonathan -- Kusnirak, Peter -- New York, N.Y. -- Science. 2007 Apr 13;316(5822):272-4. Epub 2007 Mar 8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK. s.c.lowry@qub.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17347414" 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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  • 6
    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〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 7
    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〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 8
    Electronic Resource
    Electronic Resource
    [s.l.] : Macmillian Magazines Ltd.
    Nature 428 (2004), S. 400-401 
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Dynamical resonances in the asteroid belt are the gateway for the production of near-Earth asteroids (NEAs). To generate the observed number of NEAs, however, requires the injection of many asteroids into those resonant regions. Collisional processes have long been claimed as a possible source, ...
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  • 9
    Electronic Resource
    Electronic Resource
    Amsterdam : Elsevier
    Planetary and Space Science 42 (1994), S. 345-348 
    ISSN: 0032-0633
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Geosciences , Physics
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  • 10
    Electronic Resource
    Electronic Resource
    Springer
    Earth, moon and planets 71 (1995), S. 177-187 
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract Photometric observations of 11 near-Earth asteroids were made within a regular NEA CCD photometric programme at Ondřejov Observatory in the first half of 1994. This paper shows obtained R lightcurves, V-R, R-I, and B-V color indices, and rotation preriods for 6 of them. Among the presented results, the most interesting are those for (4954) Eric, for which we obtained several high-quality lightcurves and which seems to indicate a surface heterogeneity, (1864) Daedalus, for which interesting comparison with older observations by Gehrelset al. (1971) can be made, and 1993 VW, for which the unusual color characteristics were observed. Two (1994 AW1 and 1994 GY) of the other three observed objects have fast rotations with periods of about 2.5 hours and relatively low amplitudes. Subsequent analysis of additional lightcurve data for 1994 AW1 has revealed a presence of two periods in its lightcurve (Pravecet al. 1995). The last object presented here is 1994 JF1, for which only lower limits on period and amplitude were determined.
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