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  • 1
    Publication Date: 2012-05-15
    Description: Dawn's global mapping of Vesta reveals that its observed south polar depression is composed of two overlapping giant impact features. These large basins provide exceptional windows into impact processes at planetary scales. The youngest, Rheasilvia, is 500 kilometers wide and 19 kilometers deep and finds its nearest morphologic analog among large basins on low-gravity icy satellites. Extensive ejecta deposits occur, but impact melt volume is low, exposing an unusual spiral fracture pattern that is likely related to faulting during uplift and convergence of the basin floor. Rheasilvia obliterated half of another 400-kilometer-wide impact basin, Veneneia. Both basins are unexpectedly young, roughly 1 to 2 billion years, and their formation substantially reset Vestan geology and excavated sufficient volumes of older compositionally heterogeneous crustal material to have created the Vestoids and howardite-eucrite-diogenite meteorites.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Schenk, Paul -- O'Brien, David P -- Marchi, Simone -- Gaskell, Robert -- Preusker, Frank -- Roatsch, Thomas -- Jaumann, Ralf -- Buczkowski, Debra -- McCord, Thomas -- McSween, Harry Y -- Williams, David -- Yingst, Aileen -- Raymond, Carol -- Russell, Chris -- New York, N.Y. -- Science. 2012 May 11;336(6082):694-7. doi: 10.1126/science.1223272.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Institute, Houston, TX 77058, USA. schenk@lpi.usra.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22582256" 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: 2012-05-15
    Description: Vesta is a large differentiated rocky body in the main asteroid belt that accreted within the first few million years after the formation of the earliest solar system solids. The Dawn spacecraft extensively imaged Vesta's surface, revealing a collision-dominated history. Results show that Vesta's cratering record has a strong north-south dichotomy. Vesta's northern heavily cratered terrains retain much of their earliest history. The southern hemisphere was reset, however, by two major collisions in more recent times. We estimate that the youngest of these impact structures, about 500 kilometers across, formed about 1 billion years ago, in agreement with estimates of Vesta asteroid family age based on dynamical and collisional constraints, supporting the notion that the Vesta asteroid family was formed during this event.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Marchi, S -- McSween, H Y -- O'Brien, D P -- Schenk, P -- De Sanctis, M C -- Gaskell, R -- Jaumann, R -- Mottola, S -- Preusker, F -- Raymond, C A -- Roatsch, T -- Russell, C T -- New York, N.Y. -- Science. 2012 May 11;336(6082):690-4. doi: 10.1126/science.1218757.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Lunar Science Institute, Boulder, CO, USA. marchi@boulder.swri.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22582255" 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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  • 3
    Publication Date: 2015-10-17
    Description: The Pluto system was recently explored by NASA's New Horizons spacecraft, making closest approach on 14 July 2015. Pluto's surface displays diverse landforms, terrain ages, albedos, colors, and composition gradients. Evidence is found for a water-ice crust, geologically young surface units, surface ice convection, wind streaks, volatile transport, and glacial flow. Pluto's atmosphere is highly extended, with trace hydrocarbons, a global haze layer, and a surface pressure near 10 microbars. Pluto's diverse surface geology and long-term activity raise fundamental questions about how small planets remain active many billions of years after formation. Pluto's large moon Charon displays tectonics and evidence for a heterogeneous crustal composition; its north pole displays puzzling dark terrain. Small satellites Hydra and Nix have higher albedos than expected.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stern, S A -- Bagenal, F -- Ennico, K -- Gladstone, G R -- Grundy, W M -- McKinnon, W B -- Moore, J M -- Olkin, C B -- Spencer, J R -- Weaver, H A -- Young, L A -- Andert, T -- Andrews, J -- Banks, M -- Bauer, B -- Bauman, J -- Barnouin, O S -- Bedini, P -- Beisser, K -- Beyer, R A -- Bhaskaran, S -- Binzel, R P -- Birath, E -- Bird, M -- Bogan, D J -- Bowman, A -- Bray, V J -- Brozovic, M -- Bryan, C -- Buckley, M R -- Buie, M W -- Buratti, B J -- Bushman, S S -- Calloway, A -- Carcich, B -- Cheng, A F -- Conard, S -- Conrad, C A -- Cook, J C -- Cruikshank, D P -- Custodio, O S -- Dalle Ore, C M -- Deboy, C -- Dischner, Z J B -- Dumont, P -- Earle, A M -- Elliott, H A -- Ercol, J -- Ernst, C M -- Finley, T -- Flanigan, S H -- Fountain, G -- Freeze, M J -- Greathouse, T -- Green, J L -- Guo, Y -- Hahn, M -- Hamilton, D P -- Hamilton, S A -- Hanley, J -- Harch, A -- Hart, H M -- Hersman, C B -- Hill, A -- Hill, M E -- Hinson, D P -- Holdridge, M E -- Horanyi, M -- Howard, A D -- Howett, C J A -- Jackman, C -- Jacobson, R A -- Jennings, D E -- Kammer, J A -- Kang, H K -- Kaufmann, D E -- Kollmann, P -- Krimigis, S M -- Kusnierkiewicz, D -- Lauer, T R -- Lee, J E -- Lindstrom, K L -- Linscott, I R -- Lisse, C M -- Lunsford, A W -- Mallder, V A -- Martin, N -- McComas, D J -- McNutt, R L Jr -- Mehoke, D -- Mehoke, T -- Melin, E D -- Mutchler, M -- Nelson, D -- Nimmo, F -- Nunez, J I -- Ocampo, A -- Owen, W M -- Paetzold, M -- Page, B -- Parker, A H -- Parker, J W -- Pelletier, F -- Peterson, J -- Pinkine, N -- Piquette, M -- Porter, S B -- Protopapa, S -- Redfern, J -- Reitsema, H J -- Reuter, D C -- Roberts, J H -- Robbins, S J -- Rogers, G -- Rose, D -- Runyon, K -- Retherford, K D -- Ryschkewitsch, M G -- Schenk, P -- Schindhelm, E -- Sepan, B -- Showalter, M R -- Singer, K N -- Soluri, M -- Stanbridge, D -- Steffl, A J -- Strobel, D F -- Stryk, T -- Summers, M E -- Szalay, J R -- Tapley, M -- Taylor, A -- Taylor, H -- Throop, H B -- Tsang, C C C -- Tyler, G L -- Umurhan, O M -- Verbiscer, A J -- Versteeg, M H -- Vincent, M -- Webbert, R -- Weidner, S -- Weigle, G E 2nd -- White, O L -- Whittenburg, K -- Williams, B G -- Williams, K -- Williams, S -- Woods, W W -- Zangari, A M -- Zirnstein, E -- New York, N.Y. -- Science. 2015 Oct 16;350(6258):aad1815. doi: 10.1126/science.aad1815.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, Boulder, CO 80302, USA. astern@boulder.swri.edu. ; Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA. ; National Aeronautics and Space Administration (NASA) Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. ; Southwest Research Institute, San Antonio, TX 28510, USA. ; Lowell Observatory, Flagstaff, AZ 86001, USA. ; Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA. ; Southwest Research Institute, Boulder, CO 80302, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; Universitat der Bundeswehr Munchen, Neubiberg 85577, Germany. ; Planetary Science Institute, Tucson, AZ 85719, USA. ; KinetX Aerospace, Tempe, AZ 85284, USA. ; NASA Jet Propulsion Laboratory, La Canada Flintridge, CA 91011, USA. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; University of Bonn, Bonn D-53113, Germany. ; NASA Headquarters (retired), Washington, DC 20546, USA. ; University of Arizona, Tucson, AZ 85721, USA. ; Cornell University, Ithaca, NY 14853, USA. ; NASA Headquarters, Washington, DC 20546, USA. ; Rheinisches Institut fur Umweltforschung an der Universitat zu Koln, Cologne 50931, Germany. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; Search for Extraterrestrial Intelligence Institute, Mountain View, CA 94043, USA. ; Department of Environmental Sciences, University of Virginia, Charlottesville, VA 22904, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; National Optical Astronomy Observatory, Tucson, AZ 26732, USA. ; NASA Marshall Space Flight Center, Huntsville, AL 35812, USA. ; Stanford University, Stanford, CA 94305, USA. ; Space Telescope Science Institute, Baltimore, MD 21218, USA. ; University of California, Santa Cruz, CA 95064, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Michael Soluri Photography, New York, NY 10014, USA. ; Johns Hopkins University, Baltimore, MD 21218, USA. ; Roane State Community College, Jamestown, TN 38556, USA. ; George Mason University, Fairfax, VA 22030, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26472913" 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
    Publication Date: 2016-03-19
    Description: The New Horizons mission has provided resolved measurements of Pluto's moons Styx, Nix, Kerberos, and Hydra. All four are small, with equivalent spherical diameters of ~40 kilometers for Nix and Hydra and ~10 kilometers for Styx and Kerberos. They are also highly elongated, with maximum to minimum axis ratios of ~2. All four moons have high albedos (~50 to 90%) suggestive of a water-ice surface composition. Crater densities on Nix and Hydra imply surface ages of at least 4 billion years. The small moons rotate much faster than synchronous, with rotational poles clustered nearly orthogonal to the common pole directions of Pluto and Charon. These results reinforce the hypothesis that the small moons formed in the aftermath of a collision that produced the Pluto-Charon binary.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Weaver, H A -- Buie, M W -- Buratti, B J -- Grundy, W M -- Lauer, T R -- Olkin, C B -- Parker, A H -- Porter, S B -- Showalter, M R -- Spencer, J R -- Stern, S A -- Verbiscer, A J -- McKinnon, W B -- Moore, J M -- Robbins, S J -- Schenk, P -- Singer, K N -- Barnouin, O S -- Cheng, A F -- Ernst, C M -- Lisse, C M -- Jennings, D E -- Lunsford, A W -- Reuter, D C -- Hamilton, D P -- Kaufmann, D E -- Ennico, K -- Young, L A -- Beyer, R A -- Binzel, R P -- Bray, V J -- Chaikin, A L -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Gladstone, G R -- Howett, C J A -- Linscott, I R -- Nimmo, F -- Parker, J Wm -- Philippe, S -- Protopapa, S -- Reitsema, H J -- Schmitt, B -- Stryk, T -- Summers, M E -- Tsang, C C C -- Throop, H H B -- White, O L -- Zangari, A M -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aae0030. doi: 10.1126/science.aae0030.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. hal.weaver@jhuapl.edu. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. ; Lowell Observatory, Flagstaff, AZ 86001, USA. ; National Optical Astronomy Observatory, Tucson, AZ 26732, USA. ; SETI Institute, Mountain View, CA 94043, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA. ; Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; SETI Institute, Mountain View, CA 94043, USA. Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; University of Arizona, Tucson, AZ 85721, USA. ; Independent science writer, Arlington, VT, USA. ; Southwest Research Institute, San Antonio, TX 78238, USA. ; Stanford University, Stanford, CA 94305, USA. ; University of California, Santa Cruz, CA 95064, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Roane State Community College, Oak Ridge, TN 37830, USA. ; George Mason University, Fairfax, VA 22030, USA. ; Planetary Science Institute, Tucson, AZ 85719, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989256" target="_blank"〉PubMed〈/a〉
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  • 5
    Publication Date: 2012-05-15
    Description: Vesta's surface is characterized by abundant impact craters, some with preserved ejecta blankets, large troughs extending around the equatorial region, enigmatic dark material, and widespread mass wasting, but as yet an absence of volcanic features. Abundant steep slopes indicate that impact-generated surface regolith is underlain by bedrock. Dawn observations confirm the large impact basin (Rheasilvia) at Vesta's south pole and reveal evidence for an earlier, underlying large basin (Veneneia). Vesta's geology displays morphological features characteristic of the Moon and terrestrial planets as well as those of other asteroids, underscoring Vesta's unique role as a transitional solar system body.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jaumann, R -- Williams, D A -- Buczkowski, D L -- Yingst, R A -- Preusker, F -- Hiesinger, H -- Schmedemann, N -- Kneissl, T -- Vincent, J B -- Blewett, D T -- Buratti, B J -- Carsenty, U -- Denevi, B W -- De Sanctis, M C -- Garry, W B -- Keller, H U -- Kersten, E -- Krohn, K -- Li, J-Y -- Marchi, S -- Matz, K D -- McCord, T B -- McSween, H Y -- Mest, S C -- Mittlefehldt, D W -- Mottola, S -- Nathues, A -- Neukum, G -- O'Brien, D P -- Pieters, C M -- Prettyman, T H -- Raymond, C A -- Roatsch, T -- Russell, C T -- Schenk, P -- Schmidt, B E -- Scholten, F -- Stephan, K -- Sykes, M V -- Tricarico, P -- Wagner, R -- Zuber, M T -- Sierks, H -- New York, N.Y. -- Science. 2012 May 11;336(6082):687-90. doi: 10.1126/science.1219122.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉German Aerospace Center, Institute of Planetary Research, Berlin, Germany. ralf.jaumann@dlr.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22582254" 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: 2012-09-22
    Description: We investigated the origin of unusual pitted terrain on asteroid Vesta, revealed in images from the Dawn spacecraft. Pitted terrain is characterized by irregular rimless depressions found in and around several impact craters, with a distinct morphology not observed on other airless bodies. Similar terrain is associated with numerous martian craters, where pits are thought to form through degassing of volatile-bearing material heated by the impact. Pitted terrain on Vesta may have formed in a similar manner, which indicates that portions of the surface contain a relatively large volatile component. Exogenic materials, such as water-rich carbonaceous chondrites, may be the source of volatiles, suggesting that impactor materials are preserved locally in relatively high abundance on Vesta and that impactor composition has played an important role in shaping the asteroid's geology.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Denevi, B W -- Blewett, D T -- Buczkowski, D L -- Capaccioni, F -- Capria, M T -- De Sanctis, M C -- Garry, W B -- Gaskell, R W -- Le Corre, L -- Li, J-Y -- Marchi, S -- McCoy, T J -- Nathues, A -- O'Brien, D P -- Petro, N E -- Pieters, C M -- Preusker, F -- Raymond, C A -- Reddy, V -- Russell, C T -- Schenk, P -- Scully, J E C -- Sunshine, J M -- Tosi, F -- Williams, D A -- Wyrick, D -- New York, N.Y. -- Science. 2012 Oct 12;338(6104):246-9. doi: 10.1126/science.1225374. Epub 2012 Sep 20.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA. brett.denevi@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22997131" 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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  • 7
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    German Medical Science GMS Publishing House; Düsseldorf
    In:  36. Jahrestagung der Deutschsprachigen Arbeitsgemeinschaft für Verbrennungsbehandlung (DAV 2018); 20180110-20180113; Garmisch-Partenkirchen; DOCV 66 /20180109/
    Publication Date: 2018-01-09
    Keywords: ddc: 610
    Language: German
    Type: conferenceObject
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  • 8
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    German Medical Science GMS Publishing House; Düsseldorf
    In:  Deutscher Kongress für Orthopädie und Unfallchirurgie (DKOU 2017); 20171024-20171027; Berlin; DOCWI50-967 /20171023/
    Publication Date: 2017-10-23
    Keywords: Sakrum ; Insuffizienzfraktur ; Frakturmorphologie ; ddc: 610
    Language: German
    Type: conferenceObject
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  • 9
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    German Medical Science GMS Publishing House; Düsseldorf
    In:  Deutscher Kongress für Orthopädie und Unfallchirurgie (DKOU 2017); 20171024-20171027; Berlin; DOCWI21-523 /20171023/
    Publication Date: 2017-10-23
    Keywords: Knochenqualität ; Hounsfield Units ; Osteoporose ; Osteopenie ; thorakolumbale Frakturen ; Repositionsverlust ; Cage Sinterung/Einbruch ; ddc: 610
    Language: German
    Type: conferenceObject
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  • 10
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    German Medical Science GMS Publishing House; Düsseldorf
    In:  Deutscher Kongress für Orthopädie und Unfallchirurgie (DKOU 2016); 20161025-20161028; Berlin; DOCWI39-912 /20161010/
    Publication Date: 2016-10-10
    Keywords: Sakrum ; Vertebropelvine Stabilisierung ; bisegmentale transsakrale Verschraubung ; Insuffizienzfraktur ; Osteoporose ; Outcome ; Frakturheilung ; ddc: 610
    Language: German
    Type: conferenceObject
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