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  • 1
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    High heat flow from Enceladus' south polar region measured using 10–600 cm−1 Cassini/CIRS data (2011)
    Wiley
    Details
    Publication Date: 2011-03-04
    Description: Analysis of 2008 Cassini Composite Infrared Spectrometer (CIRS) 10 to 600 cm−1 thermal emission spectra of Encleadus shows that for reasonable assumptions about the spatial distribution of the emission and the thermophysical properties of the solar-heated background surface, which are supported by CIRS observations of background temperatures at the edge of the active region, the endogenic power of Enceladus' south polar terrain is 15.8 ± 3.1 GW. This is significantly higher than the previous estimate of 5.8 ± 1.9 GW. The new value represents an improvement over the previous one, which was derived from higher wave number data (600 to 1100 cm−1) and was thus only sensitive to high-temperature emission. The mechanism capable of producing such a high endogenic power remains a mystery and challenges the current models of proposed heat production.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Convection in a volatile nitrogen-ice-rich layer drives Pluto’s geological vigour (2016)
    Springer Nature
    In: Nature
    Details
    Publication Date: 2016-06-02
    Description: Convection in a volatile nitrogen-ice-rich layer drives Pluto’s geological vigour Nature 534, 7605 (2016). doi:10.1038/nature18289 Authors: William B. McKinnon, Francis Nimmo, Teresa Wong, Paul M. Schenk, Oliver L. White, J. H. Roberts, J. M. Moore, J. R. Spencer, A. D. Howard, O. M. Umurhan, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young & K. E. Smith The vast, deep, volatile-ice-filled basin informally named Sputnik Planum is central to Pluto’s vigorous geological activity. Composed of molecular nitrogen, methane, and carbon monoxide ices, but dominated by nitrogen ice, this layer is organized into cells or polygons, typically about 10 to 40 kilometres across, that resemble the surface manifestation of solid-state convection. Here we report, on the basis of available rheological measurements, that solid layers of nitrogen ice with a thickness in excess of about one kilometre should undergo convection for estimated present-day heat-flow conditions on Pluto. More importantly, we show numerically that convective overturn in a several-kilometre-thick layer of solid nitrogen can explain the great lateral width of the cells. The temperature dependence of nitrogen-ice viscosity implies that the ice layer convects in the so-called sluggish lid regime, a unique convective mode not previously definitively observed in the Solar System. Average surface horizontal velocities of a few centimetres a year imply surface transport or renewal times of about 500,000 years, well under the ten-million-year upper-limit crater retention age for Sputnik Planum. Similar convective surface renewal may also occur on other dwarf planets in the Kuiper belt, which may help to explain the high albedos shown by some of these bodies.
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Springer Nature
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  • 3
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    Corrigendum: Convection in a volatile nitrogen-ice-rich layer drives Pluto’s geological vigour (2016)
    Springer Nature
    In: Nature
    Details
    Publication Date: 2016-09-01
    Description: Corrigendum: Convection in a volatile nitrogen-ice-rich layer drives Pluto’s geological vigour Nature 537, 7618 (2016). doi:10.1038/nature18937 Authors: William B. McKinnon, Francis Nimmo, Teresa Wong, Paul M. Schenk, Oliver L. White, J. H. Roberts, J. M. Moore, J. R. Spencer, A. D. Howard, O. M. Umurhan, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young & K. E. Smith Nature534, 82–85 (2016); doi:10.1038/nature18289In the list of the New Horizons Geology, Geophysics and Imaging Theme Team, two members were inadvertently omitted: Richard P. Binzel and Alissa Earle (both affiliated with Massachusetts Institute of Technology, Cambridge, Massachusetts
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Springer Nature
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  • 4
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    Io's thermal emission from the Galileo photopolarimeter-radiometer (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-05-20
    Description: Galileo's photopolarimeter-radiometer instrument mapped Io's thermal emission during the I24, I25, and I27 flybys with a spatial resolution of 2.2 to 300 kilometers. Mapping of Loki in I24 shows uniform temperatures for most of Loki Patera and high temperatures in the southwest corner, probably resulting from an eruption that began 1 month before the observation. Most of Loki Patera was resurfaced before I27. Pele's caldera floor has a low temperature of 160 kelvin, whereas flows at Pillan and Zamama have temperatures of up to 200 kelvin. Global maps of nighttime temperatures provide a means for estimating global heat flow.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Spencer, J R -- Rathbun, J A -- Travis, L D -- Tamppari, L K -- Barnard, L -- Martin, T Z -- McEwen, A S -- New York, N.Y. -- Science. 2000 May 19;288(5469):1198-201.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10817987" target="_blank"〉PubMed〈/a〉
    Keywords: Darkness ; Extraterrestrial Environment ; Filtration ; *Hot Temperature ; *Jupiter ; Photometry ; *Space Flight ; Sunlight ; *Volcanic Eruptions
    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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  • 5
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    Discovery of gaseous S2 in Io's Pele plume (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-05-20
    Description: Spectroscopy of Io's Pele plume against Jupiter by the Hubble Space Telescope in October 1999 revealed absorption due to S2 gas, with a column density of 1.0 +/- 0.2 x 10(16) per square centimeter, and probably also SO(2) gas with a column density of 7 +/- 3 x 10(16) per square centimeter. This SO2/S2 ratio (3 to 12) is expected from equilibration with silicate magmas near the quartz-fayalite-magnetite or wustite-magnetite buffers. Condensed S3 and S4, probable coloring agents in Pele's red plume deposits, may form by polymerization of the S2, which is unstable to ultraviolet photolysis. Diffuse red deposits near other Io volcanoes suggest that venting and polymerization of S2 gas is a widespread feature of Io volcanism.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Spencer, J R -- Jessup, K L -- McGrath, M A -- Ballester, G E -- Yelle, R -- New York, N.Y. -- Science. 2000 May 19;288(5469):1208-10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA. spencer@lowell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10817990" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; *Gases ; *Jupiter ; Spacecraft ; Spectrum Analysis ; *Sulfur ; Sulfur Dioxide ; *Volcanic Eruptions
    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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  • 6
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    Temperatures on europa from galileo photopolarimeter-radiometer: nighttime thermal anomalies (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-05-29
    Description: Galileo observations of Europa's thermal emission show low-latitude diurnal brightness temperatures in the range of 86 to 132 kelvin. Nighttime temperatures form an unexpected pattern, with high temperatures on the bright ejecta blanket of the crater Pwyll and an equatorial minimum in temperatures after sunset, uncorrelated with surface albedo or geology. The nighttime anomalies may be due to regional thermal inertia variations of an unknown origin, which are equivalent to a two- to threefold variation in thermal conductivity, or to endogenic heat fluxes locally reaching 1 watt per square meter. Endogenic heat flow at this high level, although consistent with some geological evidence, is theoretically unlikely.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Spencer -- Tamppari -- Martin -- Travis -- New York, N.Y. -- Science. 1999 May 28;284(5419):1514-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA. Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA. Goddard Institute for Space Studies, 2880 Broadway, New York, NY 10025, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10348736" 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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  • 7
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    Volcanic Activity on lo at the Time of the Ulysses Encounter (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-09-11
    Description: The population of heavy ions in lo's torus is ultimately derived from lo volcanism. Groundbased infrared observations of lo between October 1991 and March 1992, contemporaneous with the 8 February 1992 Ulysses observations of the lo torus, show that volcanic thermal emission was at the low end of the normal range at all lo longitudes during this period. In particular, the dominant hot spot Loki was quiescent. Resolved images show that there were at least four hot spots on lo's Jupiter-facing hemisphere, including Loki and a long-lived spot on the leading hemisphere (Kanehekili), of comparable 3.5-micrometer brightness but higher temperature.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Spencer, J R -- Howell, R R -- Clark, B E -- Klassen, D R -- O'connor, D -- New York, N.Y. -- Science. 1992 Sep 11;257(5076):1507-10.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17776157" 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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  • 8
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    A clathrate reservoir hypothesis for Enceladus' south polar plume (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2006-12-16
    Description: We hypothesize that active tectonic processes in the south polar terrain of Enceladus, the 500-kilometer-diameter moon of Saturn, are creating fractures that cause degassing of a clathrate reservoir to produce the plume documented by the instruments on the Cassini spacecraft. Advection of gas and ice transports energy, supplied at depth as latent heat of clathrate decomposition, to shallower levels, where it reappears as latent heat of condensation of ice. The plume itself, which has a discharge rate comparable to Old Faithful Geyser in Yellowstone National Park, probably represents small leaks from this massive advective system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kieffer, Susan W -- Lu, Xinli -- Bethke, Craig M -- Spencer, John R -- Marshak, Stephen -- Navrotsky, Alexandra -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1764-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geology, University of Illinois at Urbana-Champaign, 1301 West Green Street, Urbana, IL 61801, USA. skieffer@uiuc.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170301" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Dioxide ; Extraterrestrial Environment ; Gases ; *Ice ; Mathematics ; Methane ; Models, Theoretical ; Nitrogen ; Pressure ; *Saturn ; Spacecraft ; Temperature ; Water
    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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  • 9
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    Energetic particles in the jovian magnetotail (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    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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  • 10
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    Clump detections and limits on moons in Jupiter's ring system (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2007-10-13
    Description: The dusty jovian ring system must be replenished continuously from embedded source bodies. The New Horizons spacecraft has performed a comprehensive search for kilometer-sized moons within the system, which might have revealed the larger members of this population. No new moons were found, however, indicating a sharp cutoff in the population of jovian bodies smaller than 8-kilometer-radius Adrastea. However, the search revealed two families of clumps in the main ring: one close pair and one cluster of three to five. All orbit within a brighter ringlet just interior to Adrastea. Their properties are very different from those of the few other clumpy rings known; the origin and nonrandom distribution of these features remain unexplained, but resonant confinement by Metis may play a role.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Showalter, Mark R -- Cheng, Andrew F -- Weaver, Harold A -- Stern, S Alan -- Spencer, John R -- Throop, Henry B -- Birath, Emma M -- Rose, Debi -- Moore, Jeffrey M -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):232-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Search for Extraterrestrial Intelligence (SETI) Institute, Mountain View, CA 94043, USA. mshowalter@seti.org〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932287" 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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