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  • 1
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    In:  Pageoph, Amsterdam, Elsevier, vol. 159, no. 10, pp. 2261-2270, pp. 2083, (ISBN 1-86239-117-3)
    Publication Date: 2002
    Keywords: Modelling ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Inelastic ; Rheology ; Inversion ; Friction ; Okada ; PAG
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  • 2
    Publication Date: 2007-10-13
    Description: The New Horizons (NH) spacecraft observed Io's aurora in eclipse on four occasions during spring 2007. NH Alice ultraviolet spectroscopy and concurrent Hubble Space Telescope ultraviolet imaging in eclipse investigate the relative contribution of volcanoes to Io's atmosphere and its interaction with Jupiter's magnetosphere. Auroral brightness and morphology variations after eclipse ingress and egress reveal changes in the relative contribution of sublimation and volcanic sources to the atmosphere. Brightnesses viewed at different geometries are best explained by a dramatic difference between the dayside and nightside atmospheric density. Far-ultraviolet aurora morphology reveals the influence of plumes on Io's electrodynamic interaction with Jupiter's magnetosphere. Comparisons to detailed simulations of Io's aurora indicate that volcanoes supply 1 to 3% of the dayside atmosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Retherford, K D -- Spencer, J R -- Stern, S A -- Saur, J -- Strobel, D F -- Steffl, A J -- Gladstone, G R -- Weaver, H A -- Cheng, A F -- Parker, J Wm -- Slater, D C -- Versteeg, M H -- Davis, M W -- Bagenal, F -- Throop, H B -- Lopes, R M C -- Reuter, D C -- Lunsford, A -- Conard, S J -- Young, L A -- Moore, J M -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):237-40.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, San Antonio, TX 78228, USA. KRetherford@swri.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932289" target="_blank"〉PubMed〈/a〉
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  • 3
    Publication Date: 2007-10-13
    Description: Observations of Jupiter's nightside airglow (nightglow) and aurora obtained during the flyby of the New Horizons spacecraft show an unexpected lack of ultraviolet nightglow emissions, in contrast to the case during the Voyager flybys in 1979. The flux and average energy of precipitating electrons generally decrease with increasing local time across the nightside, consistent with a possible source region along the dusk flank of Jupiter's magnetosphere. Visible emissions associated with the interaction of Jupiter and its satellite Io extend to a surprisingly high altitude, indicating localized low-energy electron precipitation. These results indicate that the interaction between Jupiter's upper atmosphere and near-space environment is variable and poorly understood; extensive observations of the day side are no guide to what goes on at night.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gladstone, G Randall -- Stern, S Alan -- Slater, David C -- Versteeg, Maarten -- Davis, Michael W -- Retherford, Kurt D -- Young, Leslie A -- Steffl, Andrew J -- Throop, Henry -- Parker, Joel Wm -- Weaver, Harold A -- Cheng, Andrew F -- Orton, Glenn S -- Clarke, John T -- Nichols, Jonathan D -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):229-31.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, San Antonio, TX 78238, USA. rgladstone@swri.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932286" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Hydrocarbons ; Hydrogen ; *Jupiter ; Magnetics ; Spacecraft
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  • 4
    Publication Date: 2008-10-18
    Description: The study of binary Kuiper Belt objects helps to probe the dynamic conditions present during planet formation in the solar system. We report on the mutual-orbit determination of 2001 QW322, a Kuiper Belt binary with a very large separation whose properties challenge binary-formation and -evolution theories. Six years of tracking indicate that the binary's mutual-orbit period is approximately 25 to 30 years, that the orbit pole is retrograde and inclined 50 degrees to 62 degrees from the ecliptic plane, and, most surprisingly, that the mutual orbital eccentricity is 〈0.4. The semimajor axis of 105,000 to 135,000 kilometers is 10 times that of other near-equal-mass binaries. Because this weakly bound binary is prone to orbital disruption by interlopers, its lifetime in its present state is probably less than 1 billion years.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Petit, J-M -- Kavelaars, J J -- Gladman, B J -- Margot, J L -- Nicholson, P D -- Jones, R L -- Parker, J Wm -- Ashby, M L N -- Bagatin, A Campo -- Benavidez, P -- Coffey, J -- Rousselot, P -- Mousis, O -- Taylor, P A -- New York, N.Y. -- Science. 2008 Oct 17;322(5900):432-4. doi: 10.1126/science.1163148.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Observatoire de Besancon, Universite de Franche Comte, Besancon, Doubs 25010, France. petit@obs-besancon.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18927391" target="_blank"〉PubMed〈/a〉
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  • 5
    Publication Date: 2010-10-23
    Description: On 9 October 2009, the Lunar Crater Observation and Sensing Satellite (LCROSS) sent a kinetic impactor to strike Cabeus crater, on a mission to search for water ice and other volatiles expected to be trapped in lunar polar soils. The Lyman Alpha Mapping Project (LAMP) ultraviolet spectrograph onboard the Lunar Reconnaissance Orbiter (LRO) observed the plume generated by the LCROSS impact as far-ultraviolet emissions from the fluorescence of sunlight by molecular hydrogen and carbon monoxide, plus resonantly scattered sunlight from atomic mercury, with contributions from calcium and magnesium. The observed light curve is well simulated by the expansion of a vapor cloud at a temperature of ~1000 kelvin, containing ~570 kilograms (kg) of carbon monoxide, ~140 kg of molecular hydrogen, ~160 kg of calcium, ~120 kg of mercury, and ~40 kg of magnesium.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gladstone, G Randall -- Hurley, Dana M -- Retherford, Kurt D -- Feldman, Paul D -- Pryor, Wayne R -- Chaufray, Jean-Yves -- Versteeg, Maarten -- Greathouse, Thomas K -- Steffl, Andrew J -- Throop, Henry -- Parker, Joel Wm -- Kaufmann, David E -- Egan, Anthony F -- Davis, Michael W -- Slater, David C -- Mukherjee, Joey -- Miles, Paul F -- Hendrix, Amanda R -- Colaprete, Anthony -- Stern, S Alan -- New York, N.Y. -- Science. 2010 Oct 22;330(6003):472-6. doi: 10.1126/science.1186474.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, San Antonio, TX 78238, USA. rgladstone@swri.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20966244" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Monoxide ; Extraterrestrial Environment ; Hydrogen ; *Moon ; Spectrum Analysis
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  • 6
    Publication Date: 2009-10-10
    Description: We obtained Hubble Space Telescope images of 2 Pallas in September 2007 that reveal distinct color and albedo variations across the surface of this large asteroid. Pallas's shape is an ellipsoid with radii of 291 (+/-9), 278 (+/-9), and 250 (+/-9) kilometers, implying a density of 2400 (+/-250) kilograms per cubic meter-a value consistent with a body that formed from water-rich material. Our observations are consistent with the presence of an impact feature, 240 (+/-25) kilometers in diameter, within Pallas's ultraviolet-dark terrain. Our observations imply that Pallas is an intact protoplanet that has undergone impact excavation and probable internal alteration.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Schmidt, B E -- Thomas, P C -- Bauer, J M -- Li, J-Y -- McFadden, L A -- Mutchler, M J -- Radcliffe, S C -- Rivkin, A S -- Russell, C T -- Parker, J Wm -- Stern, S A -- New York, N.Y. -- Science. 2009 Oct 9;326(5950):275-8. doi: 10.1126/science.1177734.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095, USA. britneys@ucla.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19815773" target="_blank"〉PubMed〈/a〉
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  • 7
    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〉
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  • 8
    Publication Date: 2016-03-19
    Description: Observations made during the New Horizons flyby provide a detailed snapshot of the current state of Pluto's atmosphere. Whereas the lower atmosphere (at altitudes of less than 200 kilometers) is consistent with ground-based stellar occultations, the upper atmosphere is much colder and more compact than indicated by pre-encounter models. Molecular nitrogen (N2) dominates the atmosphere (at altitudes of less than 1800 kilometers or so), whereas methane (CH4), acetylene (C2H2), ethylene (C2H4), and ethane (C2H6) are abundant minor species and likely feed the production of an extensive haze that encompasses Pluto. The cold upper atmosphere shuts off the anticipated enhanced-Jeans, hydrodynamic-like escape of Pluto's atmosphere to space. It is unclear whether the current state of Pluto's atmosphere is representative of its average state--over seasonal or geologic time scales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gladstone, G Randall -- Stern, S Alan -- Ennico, Kimberly -- Olkin, Catherine B -- Weaver, Harold A -- Young, Leslie A -- Summers, Michael E -- Strobel, Darrell F -- Hinson, David P -- Kammer, Joshua A -- Parker, Alex H -- Steffl, Andrew J -- Linscott, Ivan R -- Parker, Joel Wm -- Cheng, Andrew F -- Slater, David C -- Versteeg, Maarten H -- Greathouse, Thomas K -- Retherford, Kurt D -- Throop, Henry -- Cunningham, Nathaniel J -- Woods, William W -- Singer, Kelsi N -- Tsang, Constantine C C -- Schindhelm, Eric -- Lisse, Carey M -- Wong, Michael L -- Yung, Yuk L -- Zhu, Xun -- Curdt, Werner -- Lavvas, Panayotis -- Young, Eliot F -- Tyler, G Leonard -- New Horizons Science Team -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aad8866. doi: 10.1126/science.aad8866.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Southwest Research Institute, San Antonio, TX 78238, USA. University of Texas at San Antonio, San Antonio, TX 78249, USA. rgladstone@swri.edu. ; Southwest Research Institute, Boulder, CO 80302, USA. ; National Aeronautics and Space Administration, Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. ; The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; George Mason University, Fairfax, VA 22030, USA. ; The Johns Hopkins University, Baltimore, MD 21218, USA. ; Search for Extraterrestrial Intelligence Institute, Mountain View, CA 94043, USA. ; Stanford University, Stanford, CA 94305, USA. ; Southwest Research Institute, San Antonio, TX 78238, USA. ; Southwest Research Institute, San Antonio, TX 78238, USA. University of Texas at San Antonio, San Antonio, TX 78249, USA. ; Nebraska Wesleyan University, Lincoln, NE 68504, USA. ; California Institute of Technology, Pasadena, CA 91125, USA. ; Max-Planck-Institut fur Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany. ; Groupe de Spectroscopie Moleculaire et Atmospherique, Universite Reims Champagne-Ardenne, 51687 Reims, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989258" target="_blank"〉PubMed〈/a〉
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  • 9
    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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  • 10
    Publication Date: 2016-03-19
    Description: The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile methane, carbon monoxide, and nitrogen ices that dominate Pluto's surface have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological time scales. Pluto's water ice "bedrock" was also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon's near-infrared spectra reveal highly localized areas with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Grundy, W M -- Binzel, R P -- Buratti, B J -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Ennico, K -- Howett, C J A -- Lunsford, A W -- Olkin, C B -- Parker, A H -- Philippe, S -- Protopapa, S -- Quirico, E -- Reuter, D C -- Schmitt, B -- Singer, K N -- Verbiscer, A J -- Beyer, R A -- Buie, M W -- Cheng, A F -- Jennings, D E -- Linscott, I R -- Parker, J Wm -- Schenk, P M -- Spencer, J R -- Stansberry, J A -- Stern, S A -- Throop, H B -- Tsang, C C C -- Weaver, H A -- Weigle, G E 2nd -- Young, L A -- New Horizons Science Team -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aad9189. doi: 10.1126/science.aad9189.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, Flagstaff, AZ 86001, USA. w.grundy@lowell.edu. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; NASA Jet Propulsion Laboratory, La Canada Flintridge, CA 91011, USA. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; Stanford University, Stanford, CA 94305, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Space Telescope Science Institute, Baltimore, MD, USA. ; Planetary Science Institute, Mumbai, India. ; Southwest Research Institute, San Antonio, TX 28510, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989260" target="_blank"〉PubMed〈/a〉
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