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  • American Association for the Advancement of Science (AAAS)  (14)
  • National Academy of Sciences  (1)
  • Geological Society (of London)
  • Mineralogical Society of America
  • 2005-2009  (15)
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  • 1
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    Mars north polar deposits: stratigraphy, age, and geodynamical response (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-05-17
    Description: The Shallow Radar (SHARAD) on the Mars Reconnaissance Orbiter has imaged the internal stratigraphy of the north polar layered deposits of Mars. Radar reflections within the deposits reveal a laterally continuous deposition of layers, which typically consist of four packets of finely spaced reflectors separated by homogeneous interpacket regions of nearly pure ice. The packet/interpacket structure can be explained by approximately million-year periodicities in Mars' obliquity or orbital eccentricity. The observed approximately 100-meter maximum deflection of the underlying substrate in response to the ice load implies that the present-day thickness of an equilibrium elastic lithosphere is greater than 300 kilometers. Alternatively, the response to the load may be in a transient state controlled by mantle viscosity. Both scenarios probably require that Mars has a subchondritic abundance of heat-producing elements.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Phillips, Roger J -- Zuber, Maria T -- Smrekar, Suzanne E -- Mellon, Michael T -- Head, James W -- Tanaka, Kenneth L -- Putzig, Nathaniel E -- Milkovich, Sarah M -- Campbell, Bruce A -- Plaut, Jeffrey J -- Safaeinili, Ali -- Seu, Roberto -- Biccari, Daniela -- Carter, Lynn M -- Picardi, Giovanni -- Orosei, Roberto -- Mohit, P Surdas -- Heggy, Essam -- Zurek, Richard W -- Egan, Anthony F -- Giacomoni, Emanuele -- Russo, Federica -- Cutigni, Marco -- Pettinelli, Elena -- Holt, John W -- Leuschen, Carl J -- Marinangeli, Lucia -- New York, N.Y. -- Science. 2008 May 30;320(5880):1182-5. doi: 10.1126/science.1157546. Epub 2008 May 15.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, Boulder, CO 80302, USA. roger@boulder.swri.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18483402" 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
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Mercury cratering record viewed from MESSENGER's first flyby (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: Morphologies and size-frequency distributions of impact craters on Mercury imaged during MESSENGER's first flyby elucidate the planet's geological history. Plains interior to the Caloris basin displaying color and albedo contrasts have comparable crater densities and therefore similar ages. Smooth plains exterior to Caloris exhibit a crater density approximately 40% less than on interior plains and are thus volcanic and not Caloris impact ejecta. The size distribution of smooth-plains craters matches that of lunar craters postdating the Late Heavy Bombardment, implying that the plains formed no earlier than 3.8 billion years ago (Ga). At diameters less than or equal to 8 to 10 kilometers, secondary impact craters on Mercury are more abundant than primaries; this transition diameter is much larger than that on the Moon or Mars. A low density of craters on the peak-ring basin Raditladi implies that it may be younger than 1 Ga.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Strom, Robert G -- Chapman, Clark R -- Merline, William J -- Solomon, Sean C -- Head, James W 3rd -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):79-81. doi: 10.1126/science.1159317.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. rstrom@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599774" target="_blank"〉PubMed〈/a〉
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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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    Laser altimeter observations from MESSENGER's first Mercury flyby (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    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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  • 4
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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
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
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    New perspectives on ancient Mars (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-02-26
    Description: Mars was most active during its first billion years. The core, mantle, and crust formed within approximately 50 million years of solar system formation. A magnetic dynamo in a convecting fluid core magnetized the crust, and the global field shielded a more massive early atmosphere against solar wind stripping. The Tharsis province became a focus for volcanism, deformation, and outgassing of water and carbon dioxide in quantities possibly sufficient to induce episodes of climate warming. Surficial and near-surface water contributed to regionally extensive erosion, sediment transport, and chemical alteration. Deep hydrothermal circulation accelerated crustal cooling, preserved variations in crustal thickness, and modified patterns of crustal magnetization.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Solomon, Sean C -- Aharonson, Oded -- Aurnou, Jonathan M -- Banerdt, W Bruce -- Carr, Michael H -- Dombard, Andrew J -- Frey, Herbert V -- Golombek, Matthew P -- Hauck, Steven A 2nd -- Head, James W 3rd -- Jakosky, Bruce M -- Johnson, Catherine L -- McGovern, Patrick J -- Neumann, Gregory A -- Phillips, Roger J -- Smith, David E -- Zuber, Maria T -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1214-20.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. scs@dtm.ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731435" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Climate ; Extraterrestrial Environment ; Magnetics ; *Mars ; Temperature ; Water
    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
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    Formation of glaciers on Mars by atmospheric precipitation at high obliquity (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-01-21
    Description: Surface conditions on Mars are currently cold and dry, with water ice unstable on the surface except near the poles. However, geologically recent glacierlike landforms have been identified in the tropics and the midlatitudes of Mars. The ice has been proposed to originate from either a subsurface reservoir or the atmosphere. We present high-resolution climate simulations performed with a model designed to simulate the present-day Mars water cycle but assuming a 45 degrees obliquity as experienced by Mars a few million years ago. The model predicts ice accumulation in regions where glacier landforms are observed, on the western flanks of the great volcanoes and in the eastern Hellas region. This agreement points to an atmospheric origin for the ice and reveals how precipitation could have formed glaciers on Mars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Forget, F -- Haberle, R M -- Montmessin, F -- Levrard, B -- Head, J W -- New York, N.Y. -- Science. 2006 Jan 20;311(5759):368-71.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Laboratoire de Meteorologie Dynamique, Institut Pierre Simon Laplace, Universite Paris 6 Boite Postale 99, 75252 Paris cedex 05, France. forget@lmd.jussieu.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16424337" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Climate ; Computer Simulation ; Extraterrestrial Environment ; *Ice ; *Mars ; *Water
    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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    Volcanism on Mercury: evidence from the first MESSENGER flyby (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-07-05
    Description: The origin of plains on Mercury, whether by volcanic flooding or impact ejecta ponding, has been controversial since the Mariner 10 flybys (1974-75). High-resolution images (down to 150 meters per pixel) obtained during the first MESSENGER flyby show evidence for volcanic vents around the Caloris basin inner margin and demonstrate that plains were emplaced sequentially inside and adjacent to numerous large impact craters, to thicknesses in excess of several kilometers. Radial graben and a floor-fractured crater may indicate intrusive activity. These observations, coupled with additional evidence from color images and impact crater size-frequency distributions, support a volcanic origin for several regions of plains and substantiate the important role of volcanism in the geological history of Mercury.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Head, James W -- Murchie, Scott L -- Prockter, Louise M -- Robinson, Mark S -- Solomon, Sean C -- Strom, Robert G -- Chapman, Clark R -- Watters, Thomas R -- McClintock, William E -- Blewett, David T -- Gillis-Davis, Jeffrey J -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):69-72. doi: 10.1126/science.1159256.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Brown University, Providence, RI 02912, USA. James_Head@brown.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599771" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 8
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    Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-11-22
    Description: Lobate features abutting massifs and escarpments in the middle latitudes of Mars have been recognized in images for decades, but their true nature has been controversial, with hypotheses of origin such as ice-lubricated debris flows or glaciers covered by a layer of surface debris. These models imply an ice content ranging from minor and interstitial to massive and relatively pure. Soundings of these deposits in the eastern Hellas region by the Shallow Radar on the Mars Reconnaissance Orbiter reveal radar properties entirely consistent with massive water ice, supporting the debris-covered glacier hypothesis. The results imply that these glaciers formed in a previous climate conducive to glaciation at middle latitudes. Such features may collectively represent the most extensive nonpolar ice yet recognized on Mars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Holt, John W -- Safaeinili, Ali -- Plaut, Jeffrey J -- Head, James W -- Phillips, Roger J -- Seu, Roberto -- Kempf, Scott D -- Choudhary, Prateek -- Young, Duncan A -- Putzig, Nathaniel E -- Biccari, Daniela -- Gim, Yonggyu -- New York, N.Y. -- Science. 2008 Nov 21;322(5905):1235-8. doi: 10.1126/science.1164246.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute for Geophysics, Jackson School of Geosciences, University of Texas, Austin, TX 78758, USA. jack@ig.utexas.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19023078" target="_blank"〉PubMed〈/a〉
    Keywords: *Extraterrestrial Environment ; Ice ; *Mars ; Radar
    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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  • 9
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    Spectroscopic observations of Mercury's surface reflectance during MESSENGER's first Mercury flyby (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: During MESSENGER's first flyby of Mercury, the Mercury Atmospheric and Surface Composition Spectrometer made simultaneous mid-ultraviolet to near-infrared (wavelengths of 200 to 1300 nanometers) reflectance observations of the surface. An ultraviolet absorption (〈280 nanometers) suggests that the ferrous oxide (Fe2+) content of silicates in average surface material is low (less than 2 to 3 weight percent). This result is supported by the lack of a detectable 1-micrometer Fe2+ absorption band in high-spatial-resolution spectra of mature surface materials as well as immature crater ejecta, which suggests that the ferrous iron content may be low both on the surface and at depth. Differences in absorption features and slope among the spectra are evidence for variations in composition and regolith maturation of Mercury's surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McClintock, William E -- Izenberg, Noam R -- Holsclaw, Gregory M -- Blewett, David T -- Domingue, Deborah L -- Head, James W 3rd -- Helbert, Jorn -- McCoy, Timothy J -- Murchie, Scott L -- Robinson, Mark S -- Solomon, Sean C -- Sprague, Ann L -- Vilas, Faith -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):62-5. doi: 10.1126/science.1159933.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA. william.mcclintock@lasp.colorado.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599769" target="_blank"〉PubMed〈/a〉
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  • 10
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    Return to Mercury: a global perspective on MESSENGER's first Mercury flyby (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-05
    Description: In January 2008, the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft became the first probe to fly past the planet Mercury in 33 years. The encounter revealed that Mercury is a dynamic system; its liquid iron-rich outer core is coupled through a dominantly dipolar magnetic field to the surface, exosphere, and magnetosphere, all of which interact with the solar wind. MESSENGER images confirm that lobate scarps are the dominant tectonic landform and record global contraction associated with cooling of the planet. The history of contraction can be related to the history of volcanism and cratering, and the total contractional strain is at least one-third greater than inferred from Mariner 10 images. On the basis of measurements of thermal neutrons made during the flyby, the average abundance of iron in Mercury's surface material is less than 6% by weight.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Solomon, Sean C -- McNutt, Ralph L Jr -- Watters, Thomas R -- Lawrence, David J -- Feldman, William C -- Head, James W -- Krimigis, Stamatios M -- Murchie, Scott L -- Phillips, Roger J -- Slavin, James A -- Zuber, Maria T -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):59-62. doi: 10.1126/science.1159706.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. scs@dtm.ciw.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599768" target="_blank"〉PubMed〈/a〉
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