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  • 1
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    The elemental composition of asteroid 433 eros: results of the NEAR-shoemaker X-ray spectrometer (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-09-23
    Description: We report major element composition ratios for regions of the asteroid 433 Eros imaged during two solar flares and quiet sun conditions during the period of May to July 2000. Low aluminum abundances for all regions argue against global differentiation of Eros. Magnesium/silicon, aluminum/silicon, calcium/silicon, and iron/silicon ratios are best interpreted as a relatively primitive, chondritic composition. Marked depletions in sulfur and possible aluminum and calcium depletions, relative to ordinary chondrites, may represent signatures of limited partial melting or impact volatilization.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Trombka -- Squyres -- Bruckner -- Boynton -- Reedy -- McCoy -- Gorenstein -- Evans -- Arnold -- Starr -- Nittler -- Murphy -- Mikheeva I -- McNutt Jr -- McClanahan -- McCartney -- Goldsten -- Gold -- Floyd -- Clark -- Burbine -- Bhangoo -- Bailey -- Petaev -- New York, N.Y. -- Science. 2000 Sep 22;289(5487):2101-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Goddard Space Flight Center, Code 691, Greenbelt, MD 20771, USA. Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. Max-Planck-Institut fur Chemie, Postfach 3060, D-55020 Mainz, Germany. Department of Planetary Science, Spac.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11000107" 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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    Energetic particles in the jovian magnetotail (2007)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2007-10-13
    Description: When the solar wind hits Jupiter's magnetic field, it creates a long magnetotail trailing behind the planet that channels material out of the Jupiter system. The New Horizons spacecraft traversed the length of the jovian magnetotail to 〉2500 jovian radii (RJ; 1 RJ identical with 71,400 kilometers), observing a high-temperature, multispecies population of energetic particles. Velocity dispersions, anisotropies, and compositional variation seen in the deep-tail (greater, similar 500 RJ) with a approximately 3-day periodicity are similar to variations seen closer to Jupiter in Galileo data. The signatures suggest plasma streaming away from the planet and injection sites in the near-tail region (approximately 200 to 400 RJ) that could be related to magnetic reconnection events. The tail structure remains coherent at least until it reaches the magnetosheath at 1655 RJ.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McNutt, R L Jr -- Haggerty, D K -- Hill, M E -- Krimigis, S M -- Livi, S -- Ho, G C -- Gurnee, R S -- Mauk, B H -- Mitchell, D G -- Roelof, E C -- McComas, D J -- Bagenal, F -- Elliott, H A -- Brown, L E -- Kusterer, M -- Vandegriff, J -- Stern, S A -- Weaver, H A -- Spencer, J R -- Moore, J M -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):220-2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. ralph.mcnutt@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932283" target="_blank"〉PubMed〈/a〉
    Keywords: Electrons ; Extraterrestrial Environment ; Ions ; *Jupiter ; Oxygen ; Protons ; Spacecraft ; Sulfur ; Temperature
    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
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    Mercury's magnetosphere after MESSENGER's first flyby (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: Observations by MESSENGER show that Mercury's magnetosphere is immersed in a comet-like cloud of planetary ions. The most abundant, Na+, is broadly distributed but exhibits flux maxima in the magnetosheath, where the local plasma flow speed is high, and near the spacecraft's closest approach, where atmospheric density should peak. The magnetic field showed reconnection signatures in the form of flux transfer events, azimuthal rotations consistent with Kelvin-Helmholtz waves along the magnetopause, and extensive ultralow-frequency wave activity. Two outbound current sheet boundaries were observed, across which the magnetic field decreased in a manner suggestive of a double magnetopause. The separation of these current layers, comparable to the gyro-radius of a Na+ pickup ion entering the magnetosphere after being accelerated in the magnetosheath, may indicate a planetary ion boundary layer.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Slavin, James A -- Acuna, Mario H -- Anderson, Brian J -- Baker, Daniel N -- Benna, Mehdi -- Gloeckler, George -- Gold, Robert E -- Ho, George C -- Killen, Rosemary M -- Korth, Haje -- Krimigis, Stamatios M -- McNutt, Ralph L Jr -- Nittler, Larry R -- Raines, Jim M -- Schriver, David -- Solomon, Sean C -- Starr, Richard D -- Travnicek, Pavel -- Zurbuchen, Thomas H -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):85-9. doi: 10.1126/science.1159040.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. james.a.slavin@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599776" 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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  • 4
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    Laser altimeter observations from MESSENGER's first Mercury flyby (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-07-05
    Description: A 3200-kilometers-long profile of Mercury by the Mercury Laser Altimeter on the MESSENGER spacecraft spans approximately 20% of the near-equatorial region of the planet. Topography along the profile is characterized by a 5.2-kilometer dynamic range and 930-meter root-mean-square roughness. At long wavelengths, topography slopes eastward by 0.02 degrees , implying a variation of equatorial shape that is at least partially compensated. Sampled craters on Mercury are shallower than their counterparts on the Moon, at least in part the result of Mercury's higher gravity. Crater floors vary in roughness and slope, implying complex modification over a range of length scales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Zuber, Maria T -- Smith, David E -- Solomon, Sean C -- Phillips, Roger J -- Peale, Stanton J -- Head, James W 3rd -- Hauck, Steven A 2nd -- McNutt, Ralph L Jr -- Oberst, Jurgen -- Neumann, Gregory A -- Lemoine, Frank G -- Sun, Xiaoli -- Barnouin-Jha, Olivier -- Harmon, John K -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):77-9. doi: 10.1126/science.1159086.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA. zuber@mit.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599773" 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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    MESSENGER observations of the composition of Mercury's ionized exosphere and plasma environment (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: The region around Mercury is filled with ions that originate from interactions of the solar wind with Mercury's space environment and through ionization of its exosphere. The MESSENGER spacecraft's observations of Mercury's ionized exosphere during its first flyby yielded Na+, O+, and K+ abundances, consistent with expectations from observations of neutral species. There are increases in ions at a mass per charge (m/q) = 32 to 35, which we interpret to be S+ and H2S+, with (S+ + H2S+)/(Na+ + Mg+) = 0.67 +/- 0.06, and from water-group ions around m/q = 18, at an abundance of 0.20 +/- 0.03 relative to Na+ plus Mg+. The fluxes of Na+, O+, and heavier ions are largest near the planet, but these Mercury-derived ions fill the magnetosphere. Doubly ionized ions originating from Mercury imply that electrons with energies less than 1 kiloelectron volt are substantially energized in Mercury's magnetosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Zurbuchen, Thomas H -- Raines, Jim M -- Gloeckler, George -- Krimigis, Stamatios M -- Slavin, James A -- Koehn, Patrick L -- Killen, Rosemary M -- Sprague, Ann L -- McNutt, Ralph L Jr -- Solomon, Sean C -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):90-2. doi: 10.1126/science.1159314.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143, USA. thomasz@umich.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599777" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 6
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    Reflectance and color variations on Mercury: regolith processes and compositional heterogeneity (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: Multispectral images of Mercury obtained by the MESSENGER spacecraft reveal that its surface has an overall relatively low reflectance with three large-scale units identified on the basis of reflectance and slope (0.4 to 1.0 micrometer). A higher-reflectance, relatively red material occurs as a distinct class of smooth plains that were likely emplaced volcanically; a lower-reflectance material with a lesser spectral slope may represent a distinct crustal component enriched in opaque minerals, possibly more common at depth. A spectrally intermediate terrain probably forms most of the upper crust. Three other spectrally distinct but spatially restricted units include fresh crater ejecta less affected by space weathering than other surface materials; high-reflectance deposits seen in some crater floors; and moderately high-reflectance, relatively reddish material associated with rimless depressions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Robinson, Mark S -- Murchie, Scott L -- Blewett, David T -- Domingue, Deborah L -- Hawkins, S Edward 3rd -- Head, James W -- Holsclaw, Gregory M -- McClintock, William E -- McCoy, Timothy J -- McNutt, Ralph L Jr -- Prockter, Louise M -- Solomon, Sean C -- Watters, Thomas R -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):66-9. doi: 10.1126/science.1160080.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA. robinson@ser.asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599770" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 7
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    The major-element composition of Mercury's surface from MESSENGER X-ray spectrometry (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-10-01
    Description: X-ray fluorescence spectra obtained by the MESSENGER spacecraft orbiting Mercury indicate that the planet's surface differs in composition from those of other terrestrial planets. Relatively high Mg/Si and low Al/Si and Ca/Si ratios rule out a lunarlike feldspar-rich crust. The sulfur abundance is at least 10 times higher than that of the silicate portion of Earth or the Moon, and this observation, together with a low surface Fe abundance, supports the view that Mercury formed from highly reduced precursor materials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particles. Low Fe and Ti abundances do not support the proposal that opaque oxides of these elements contribute substantially to Mercury's low and variable surface reflectance.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nittler, Larry R -- Starr, Richard D -- Weider, Shoshana Z -- McCoy, Timothy J -- Boynton, William V -- Ebel, Denton S -- Ernst, Carolyn M -- Evans, Larry G -- Goldsten, John O -- Hamara, David K -- Lawrence, David J -- McNutt, Ralph L Jr -- Schlemm, Charles E 2nd -- Solomon, Sean C -- Sprague, Ann L -- New York, N.Y. -- Science. 2011 Sep 30;333(6051):1847-50. doi: 10.1126/science.1211567.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. lnittler@ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21960623" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 8
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    The global magnetic field of Mercury from MESSENGER orbital observations (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-10-01
    Description: Magnetometer data acquired by the MESSENGER spacecraft in orbit about Mercury permit the separation of internal and external magnetic field contributions. The global planetary field is represented as a southward-directed, spin-aligned, offset dipole centered on the spin axis. Positions where the cylindrical radial magnetic field component vanishes were used to map the magnetic equator and reveal an offset of 484 +/- 11 kilometers northward of the geographic equator. The magnetic axis is tilted by less than 3 degrees from the rotation axis. A magnetopause and tail-current model was defined by using 332 magnetopause crossing locations. Residuals of the net external and offset-dipole fields from observations north of 30 degrees N yield a best-fit planetary moment of 195 +/- 10 nanotesla-R(M)(3), where R(M) is Mercury's mean radius.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Anderson, Brian J -- Johnson, Catherine L -- Korth, Haje -- Purucker, Michael E -- Winslow, Reka M -- Slavin, James A -- Solomon, Sean C -- McNutt, Ralph L Jr -- Raines, Jim M -- Zurbuchen, Thomas H -- New York, N.Y. -- Science. 2011 Sep 30;333(6051):1859-62. doi: 10.1126/science.1211001.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. brian.anderson@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21960627" target="_blank"〉PubMed〈/a〉
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  • 9
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    Radioactive elements on Mercury's surface from MESSENGER: implications for the planet's formation and evolution (2011)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2011-10-01
    Description: The MESSENGER Gamma-Ray Spectrometer measured the average surface abundances of the radioactive elements potassium (K, 1150 +/- 220 parts per million), thorium (Th, 220 +/- 60 parts per billion), and uranium (U, 90 +/- 20 parts per billion) in Mercury's northern hemisphere. The abundance of the moderately volatile element K, relative to Th and U, is inconsistent with physical models for the formation of Mercury requiring extreme heating of the planet or its precursor materials, and supports formation from volatile-containing material comparable to chondritic meteorites. Abundances of K, Th, and U indicate that internal heat production has declined substantially since Mercury's formation, consistent with widespread volcanism shortly after the end of late heavy bombardment 3.8 billion years ago and limited, isolated volcanic activity since.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Peplowski, Patrick N -- Evans, Larry G -- Hauck, Steven A 2nd -- McCoy, Timothy J -- Boynton, William V -- Gillis-Davis, Jeffery J -- Ebel, Denton S -- Goldsten, John O -- Hamara, David K -- Lawrence, David J -- McNutt, Ralph L Jr -- Nittler, Larry R -- Solomon, Sean C -- Rhodes, Edgar A -- Sprague, Ann L -- Starr, Richard D -- Stockstill-Cahill, Karen R -- New York, N.Y. -- Science. 2011 Sep 30;333(6051):1850-2. doi: 10.1126/science.1211576.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. patrick.peplowski@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21960624" target="_blank"〉PubMed〈/a〉
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  • 10
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    The final end of the final frontier? (2012)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2012-12-01
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lisse, Carey Michael -- McNutt, Ralph L Jr -- New York, N.Y. -- Science. 2012 Nov 30;338(6111):1149-50. doi: 10.1126/science.338.6111.1149-b.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23197514" target="_blank"〉PubMed〈/a〉
    Keywords: Budgets ; Capital Financing ; Government Programs/*economics ; *Planets ; Robotics/economics/methods ; Space Flight/*economics/methods ; United States ; United States National Aeronautics and Space Administration/*economics
    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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