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  • 1
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    Cryovolcanism on Titan: New results from Cassini RADAR and VIMS (2013)
    Wiley
    Details
    Publication Date: 2013-02-13
    Description: : [1]  The existence of cryovolcanic features on Titan has been the subject of some controversy. Here we use observations from the Cassini RADAR, including SAR imaging, radiometry,and topographic data, as well as compositional data from the Visible and Infrared Spectrometer (VIMS) to re-examine several putative cryovolcanic features on Titan in terms of likely processes of origin (fluvial, cryovolcanic, or other). We present evidence to support the cryovolcanic origin of features in the region formerly known as Sotra Facula, which includes the deepest pit so far found on Titan (now known as Sotra patera), flow-like features (Mohini Fluctus) and some of the highest mountains on Titan (Doom and Erebor Montes). We interpret this region to be a cryovolcanic complex of multiple cones, craters, and flows. However, we find that some other previously supposed cryovolcanic features were likely formed by other processes. Cryovolcanism is still a possible formation mechanism for several features, including the flow-like units in Hotei Regio. We discuss implications for eruption style and composition of cryovolcanism on Titan. Our analysis shows the great value of combining data sets when interpreting Titan's geology and in particular stresses the value of RADAR stereogrammetry when combined with SAR imaging and VIMS.
    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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    An upper limit for ice in Shackleton crater as revealed by LRO Mini-RF orbital radar (2012)
    Wiley
    Details
    Publication Date: 2012-07-28
    Description: Although diverse measurements have indicated H+, OH−, or H2O species in the lunar polar regions, pinpointing its location, form, and abundance in specific reservoirs has proven elusive. Here we report on the first orbital radar measurements of Shackleton crater near the lunar south pole. Mini-RF observations indicate a patchy, heterogeneous enhancement in CPR (circular polarization ratio) on the crater walls whose strength decreases with depth toward the crater floor, a result that is most consistent with a roughness effect due to less mature regolith present on the crater wall slopes. However, the results do not rule out a modest ice contribution, and an upper limit of ∼5–10 wt% H2O ice (up to 30 vol.%) present in the uppermost meter of regolith is also consistent with the observations.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    The location of Airy-0, the Mars prime meridian reference, from stereo photogrammetric processing of THEMIS IR imaging and digital elevation data (2014)
    Wiley
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    Publication Date: 2014-11-13
    Description: The small crater Airy-0 was selected from Mariner 9 images to be the reference for the Mars prime meridian. Initial analyses in the year 2000 tied Viking Orbiter and Mars Orbiter Camera images of Airy-0 to the evolving Mars Orbiter Laser Altimeter global digital terrain model to update the location of Airy-0. Based upon this tie and radiometric tracking of landers / rovers from earth, new expressions for the Mars spin axis direction, spin rate and prime meridian epoch value were produced to define the orientation of the Martian surface in inertial space over time. Since the Mars Global Surveyor mission and Mars Orbiter Laser Altimeter global digital terrain model were completed some time ago, a more exhaustive study has been performed to determine the accuracy of the Airy-0 location and orientation of Mars at the standard epoch. THEMIS IR image cubes of the Airy and Gale crater regions were tied to the global terrain grid using precision stereo photogrammetric image proce ssing techniques. The Airy-0 location was determined to be about 0.001 ∘ east of its predicted location using the currently defined IAU prime meridian location. Information on this new location and how it was derived will be provided to the NASA Mars Exploration Program Geodesy and Cartography Working Group for their assessment. This NASA group will make a recommendation to the IAU Working Group on Cartographic Coordinates and Rotational Elements to update the expression for the Mars spin axis direction, spin rate and prime meridian location.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 4
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    Observations of comet 19P/Borrelly by the miniature integrated camera and spectrometer aboard Deep Space 1 (2002)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2002-04-06
    Description: The nucleus of the Jupiter-family comet 19P/Borrelly was closely observed by the Miniature Integrated Camera and Spectrometer aboard the Deep Space 1 spacecraft on 22 September 2001. The 8-kilometer-long body is highly variegated on a scale of 200 meters, exhibiting large albedo variations (0.01 to 0.03) and complex geologic relationships. Short-wavelength infrared spectra (1.3 to 2.6 micrometers) show a slope toward the red and a hot, dry surface (〈/=345 kelvin, with no trace of water ice or hydrated minerals), consistent with approximately 10% or less of the surface actively sublimating. Borrelly's coma exhibits two types of dust features: fans and highly collimated jets. At encounter, the near-nucleus coma was dominated by a prominent dust jet that resolved into at least three smaller jets emanating from a broad basin in the middle of the nucleus. Because the major dust jet remained fixed in orientation, it is evidently aligned near the rotation axis of the nucleus.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Soderblom, L A -- Becker, T L -- Bennett, G -- Boice, D C -- Britt, D T -- Brown, R H -- Buratti, B J -- Isbell, C -- Giese, B -- Hare, T -- Hicks, M D -- Howington-Kraus, E -- Kirk, R L -- Lee, M -- Nelson, R M -- Oberst, J -- Owen, T C -- Rayman, M D -- Sandel, B R -- Stern, S A -- Thomas, N -- Yelle, R V -- New York, N.Y. -- Science. 2002 May 10;296(5570):1087-91. Epub 2002 Apr 4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉United States Geological Survey, 2255 North Gemini Drive, Flagstaff, AZ 86001, USA. lsoderblom@usgs.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11934989" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon/analysis ; Cosmic Dust ; Hydrocarbons/analysis ; *Meteoroids ; Spectrum Analysis ; Temperature
    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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    Subsurface energy storage and transport for solar-powered geysers on triton (1990)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1990-10-19
    Description: The location of active geyser-like eruptions and related features close to the current subsolar latitude on Triton suggests a solar energy source for these phenomena. Solidstate greenhouse calculations have shown that sunlight can generate substantially elevated subsurface temperatures. A variety of models for the storage of solar energy in a sub-greenhouse layer and for the supply of gas and energy to a geyser are examined. "Leaky greenhouse" models with only vertical gas transport are inconsistent with the observed upper limit on geyser radius of approximately 1.5 kilometers. However, lateral transport of energy by gas flow in a porous N(2) layer with a block size on the order of a meter can supply the required amount of gas to a source region approximately 1 kilometer in radius. The decline of gas output to steady state may occur over a period comparable with the inferred active geyser lifetime of five Earth years. The required subsurface permeability may be maintained by thermal fracturing of the residual N2 polar cap. A lower limit on geyser source radius of approximately 50 to 100 meters predicted by a theory of negatively buoyant jets is not readily attained.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kirk, R L -- Brown, R H -- Soderblom, L A -- New York, N.Y. -- Science. 1990 Oct 19;250(4979):424-9.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17793019" 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
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    Triton's Geyser-Like Plumes: Discovery and Basic Characterization (1990)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1990-10-19
    Description: At least four active geyser-like eruptions were discovered in Voyager 2 images of Triton, Neptune's large satellite. The two best documented eruptions occur as columns of dark material rising to an altitude of about 8 kilometers where dark clouds of material are left suspended to drift downwind over 100 kilometers. The radii of the rising columns appear to be in the range of several tens of meters to a kilometer. One model for the mechanism to drive the plumes involves heating of nitrogen ice in a subsurface greenhouse environment; nitrogen gas pressurized by the solar heating explosively vents to the surface carrying clouds of ice and dark partides into the atmosphere. A temperature increase of less than 4 kelvins above the ambient surface value of 38 +/- 3 kelvins is more than adequate to drive the plumes to an 8-kilometer altitude. The mass flux in the trailing clouds is estimated to consist of up to 10 kilograms of fine dark particles per second or twice as much nitrogen ice and perhaps several hundred or more kilograms of nitrogen gas per second. Each eruption may last a year or more, during which on the order of a tenth of a cubic kilometer of ice is sublimed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Soderblom, L A -- Kieffer, S W -- Becker, T L -- Brown, R H -- Cook, A F 2nd -- Hansen, C J -- Johnson, T V -- Kirk, R L -- Shoemaker, E M -- New York, N.Y. -- Science. 1990 Oct 19;250(4979):410-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17793016" 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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    Energy Sources for Triton's Geyser-Like Plumes (1990)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1990-10-19
    Description: Four geyser-like plumes were discovered near Triton's south pole in areas now in permanent sunlight. Because Triton's southern hemisphere is nearing a maximum summer solstice, insolation as a driver or a trigger for Triton's geyser-like plumes is an attractive hypothesis. Trapping of solar radiation in a translucent, low-conductivity surface layer (in a solid-state greenhouse), which is subsequently released in the form of latent heat of sublimation, could provide the required energy. Both the classical solid-state greenhouse consisting of exponentially absorbed insolation in a gray, translucent layer of solid nitrogen, and the "super" greenhouse consisting of a relatively transparent solid-nitrogen layer over an opaque, absorbing layer are plausible candidates. Geothermal heat may also play a part if assisted by the added energy input of seasonal cycles of insolation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Brown, R H -- Kirk, R L -- Johnson, T V -- Soderblom, L A -- New York, N.Y. -- Science. 1990 Oct 19;250(4979):431-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17793021" 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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  • 8
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    Titan's rotation reveals an internal ocean and changing zonal winds (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-03-22
    Description: Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present-day rotation period difference from synchronous spin leads to a shift of approximately 0.36 degrees per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating atmosphere, but only if Titan's crust is decoupled from the core by an internal water ocean like that on Europa.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lorenz, Ralph D -- Stiles, Bryan W -- Kirk, Randolph L -- Allison, Michael D -- Del Marmo, Paolo Persi -- Iess, Luciano -- Lunine, Jonathan I -- Ostro, Steven J -- Hensley, Scott -- Intramural NIH HHS/ -- New York, N.Y. -- Science. 2008 Mar 21;319(5870):1649-51. doi: 10.1126/science.1151639.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Department, Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ralph.lorenz@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18356521" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; Ice ; *Saturn ; Spacecraft ; *Water ; Wind
    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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  • 9
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    Size and shape of Saturn's moon Titan (2009)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2009-04-04
    Description: Cassini observations show that Saturn's moon Titan is slightly oblate. A fourth-order spherical harmonic expansion yields north polar, south polar, and mean equatorial radii of 2574.32 +/- 0.05 kilometers (km), 2574.36 +/- 0.03 km, and 2574.91 +/- 0.11 km, respectively; its mean radius is 2574.73 +/- 0.09 km. Titan's shape approximates a hydrostatic, synchronously rotating triaxial ellipsoid but is best fit by such a body orbiting closer to Saturn than Titan presently does. Titan's lack of high relief implies that most--but not all--of the surface features observed with the Cassini imaging subsystem and synthetic aperture radar are uncorrelated with topography and elevation. Titan's depressed polar radii suggest that a constant geopotential hydrocarbon table could explain the confinement of the hydrocarbon lakes to high latitudes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Zebker, Howard A -- Stiles, Bryan -- Hensley, Scott -- Lorenz, Ralph -- Kirk, Randolph L -- Lunine, Jonathan -- New York, N.Y. -- Science. 2009 May 15;324(5929):921-3. doi: 10.1126/science.1168905. Epub 2009 Apr 2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geophysics, Stanford University, Stanford, CA 94305, USA. zebker@stanford.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19342551" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Hydrocarbons ; *Saturn
    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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    Results from the Mars Pathfinder camera (1997)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1997
    Description: Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmospheric haze (opacity approximately 0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, P H -- Bell, J F 3rd -- Bridges, N T -- Britt, D T -- Gaddis, L -- Greeley, R -- Keller, H U -- Herkenhoff, K E -- Jaumann, R -- Johnson, J R -- Kirk, R L -- Lemmon, M -- Maki, J N -- Malin, M C -- Murchie, S L -- Oberst, J -- Parker, T J -- Reid, R J -- Sablotny, R -- Soderblom, L A -- Stoker, C -- Sullivan, R -- Thomas, N -- Tomasko, M G -- Wegryn, E -- New York, N.Y. -- Science. 1997 Dec 5;278(5344):1758-65.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. psmith@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9388170" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment ; Ice ; *Mars ; Minerals ; *Water ; Wind
    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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