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  • 1
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    Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations (2011)
    Wiley
    Details
    Publication Date: 2011-07-07
    Description: Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity.
    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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    Galileo at Io: results from high-resolution imaging (2000)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2000-05-20
    Description: During late 1999/early 2000, the solid state imaging experiment on the Galileo spacecraft returned more than 100 high-resolution (5 to 500 meters per pixel) images of volcanically active Io. We observed an active lava lake, an active curtain of lava, active lava flows, calderas, mountains, plateaus, and plains. Several of the sulfur dioxide-rich plumes are erupting from distal flows, rather than from the source of silicate lava (caldera or fissure, often with red pyroclastic deposits). Most of the active flows in equatorial regions are being emplaced slowly beneath insulated crust, but rapidly emplaced channelized flows are also found at all latitudes. There is no evidence for high-viscosity lava, but some bright flows may consist of sulfur rather than mafic silicates. The mountains, plateaus, and calderas are strongly influenced by tectonics and gravitational collapse. Sapping channels and scarps suggest that many portions of the upper approximately 1 kilometer are rich in volatiles.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McEwen, A S -- Belton, M J -- Breneman, H H -- Fagents, S A -- Geissler, P -- Greeley, R -- Head, J W -- Hoppa, G -- Jaeger, W L -- Johnson, T V -- Keszthelyi, L -- Klaasen, K P -- Lopes-Gautier, R -- Magee, K P -- Milazzo, M P -- Moore, J M -- Pappalardo, R T -- Phillips, C B -- Radebaugh, J -- Schubert, G -- Schuster, P -- Simonelli, D P -- Sullivan, R -- Thomas, P C -- Turtle, E P -- Williams, D A -- New York, N.Y. -- Science. 2000 May 19;288(5469):1193-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10817986" target="_blank"〉PubMed〈/a〉
    Keywords: *Extraterrestrial Environment ; Geological Phenomena ; Geology ; Image Enhancement ; *Jupiter ; *Space Flight ; Spectrophotometry, Infrared ; *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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  • 3
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    Galileo encounter with 951 gaspra: first pictures of an asteroid (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-09-18
    Description: Galileo images of Gaspra reveal it to be an irregularly shaped object (19 by 12 by 11 kilometers) that appears to have been created by a catastrophic collisional disruption of a precursor parent body. The cratering age of the surface is about 200 million years. Subtle albedo and color variations appear to correlate with morphological features: Brighter materials are associated with craters especially along the crests of ridges, have a stronger 1-micrometer absorption, and may represent freshly excavated mafic materials; darker materials exhibiting a significantly weaker 1-micrometer absorption appear concentrated in interridge areas. One explanation of these patterns is that Gaspra is covered with a thin regolith and that some of this material has migrated downslope in some areas.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Belton, M J -- Veverka, J -- Thomas, P -- Helfenstein, P -- Simonelli, D -- Chapman, C -- Davies, M E -- Greeley, R -- Greenberg, R -- Head, J -- Murchie, S -- Klaasen, K -- Johnson, T V -- McEwen, A -- Morrison, D -- Neukum, G -- Fanale, F -- Anger, C -- Carr, M -- Pilcher, C -- New York, N.Y. -- Science. 1992 Sep 18;257(5077):1647-52.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17841160" 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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  • 4
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    Images from galileo of the venus cloud deck (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-09-27
    Description: Images of Venus taken at 418 (violet) and 986 [near-infrared (NIR)] nanometers show that the morphology and motions of large-scale features change with depth in the cloud deck. Poleward meridional velocities, seen in both spectral regions, are much reduced in the NIR In the south polar region the markings in the two wavelength bands are strongly anticorrelated. The images follow the changing state of the upper cloud layer downwind of the subsolar point, and the zonal flow field shows a longitudinal periodicity that may be coupled to the formation of large-scale planetary waves. No optical lightning was detected.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Belton, M J -- Gierasch, P J -- Smith, M D -- Helfenstein, P -- Schinder, P J -- Pollack, J B -- Rages, K A -- Ingersoll, A P -- Klaasen, K P -- Veverka, J -- Anger, C D -- Carr, M H -- Chapman, C R -- Davies, M E -- Fanale, F P -- Greeley, R -- Greenberg, R -- Head, J W 3rd -- Morrison, D -- Neukum, G -- Pilcher, C B -- New York, N.Y. -- Science. 1991 Sep 27;253(5027):1531-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17784096" 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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    Magma generation on Mars: amounts, rates, and comparisons with Earth, moon, and venus (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-11-15
    Description: Total extrusive and intrusive magma generated on Mars over the last approximately 3.8 billion years is estimated at 654 x 10(6) cubic kilometers, or 0.17 cubic kilometers per year (km(3)/yr), substantially less than rates for Earth (26 to 34 km(3)/yr) and Venus (less than 20 km(3)/yr) but much more than for the Moon (0.025 km(3)/yr). When scaled to Earth's mass the martian rate is much smaller than that for Earth or Venus and slightly smaller than for the Moon.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Greeley, R -- Schneid, B D -- New York, N.Y. -- Science. 1991 Nov 15;254(5034):996-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17731523" 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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    Lunar impact basins and crustal heterogeneity: new Western limb and far side data from galileo (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-01-31
    Description: Multispectral images of the lunar western limb and far side obtained from Galileo reveal the compositional nature of several prominent lunar features and provide new information on lunar evolution. The data reveal that the ejecta from the Orientale impact basin (900 kilometers in diameter) lying outside the Cordillera Mountains was excavated from the crust, not the mantle, and covers pre-Orientale terrain that consisted of both highland materials and relatively large expanses of ancient mare basalts. The inside of the far side South Pole-Aitken basin (〉2000 kilometers in diameter) has low albedo, red color, and a relatively high abundance of iron- and magnesium-rich materials. These features suggest that the impact may have penetrated into the deep crust or lunar mantle or that the basin contains ancient mare basalts that were later covered by highlands ejecta.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Belton, M J -- Head, J W 3rd -- Pieters, C M -- Greeley, R -- McEwen, A S -- Neukum, G -- Klaasen, K P -- Anger, C D -- Carr, M H -- Chapman, C R -- Davies, M E -- Fanale, F P -- Gierasch, P J -- Greenberg, R -- Ingersoll, A P -- Johnson, T -- Paczkowski, B -- Pilcher, C B -- Veverka, J -- New York, N.Y. -- Science. 1992 Jan 31;255(5044):570-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17792379" 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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    Results from the Mars Pathfinder camera (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    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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  • 8
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    Atmospheric imaging results from the Mars exploration rovers: Spirit and Opportunity (2004)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2004-12-04
    Description: A visible atmospheric optical depth of 0.9 was measured by the Spirit rover at Gusev crater and by the Opportunity rover at Meridiani Planum. Optical depth decreased by about 0.6 to 0.7% per sol through both 90-sol primary missions. The vertical distribution of atmospheric dust at Gusev crater was consistent with uniform mixing, with a measured scale height of 11.56 +/- 0.62 kilometers. The dust's cross section weighted mean radius was 1.47 +/- 0.21 micrometers (mm) at Gusev and 1.52 +/- 0.18 mm at Meridiani. Comparison of visible optical depths with 9-mm optical depths shows a visible-to-infrared optical depth ratio of 2.0 +/- 0.2 for comparison with previous monitoring of infrared optical depths.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lemmon, M T -- Wolff, M J -- Smith, M D -- Clancy, R T -- Banfield, D -- Landis, G A -- Ghosh, A -- Smith, P H -- Spanovich, N -- Whitney, B -- Whelley, P -- Greeley, R -- Thompson, S -- Bell, J F 3rd -- Squyres, S W -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1753-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Texas A&M University, College Station, TX 77843, USA. lemmon@tamu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576613" target="_blank"〉PubMed〈/a〉
    Keywords: Algorithms ; Atmosphere ; Carbon Dioxide ; Extraterrestrial Environment ; *Mars ; Solar System ; Spacecraft ; 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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  • 9
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    Wind-related processes detected by the Spirit Rover at Gusev Crater, Mars (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: Wind-abraded rocks, ripples, drifts, and other deposits of windblown sediments are seen at the Columbia Memorial Station where the Spirit rover landed. Orientations of these features suggest formative winds from the north-northwest, consistent with predictions from atmospheric models of afternoon winds in Gusev Crater. Cuttings from the rover Rock Abrasion Tool are asymmetrically distributed toward the south-southeast, suggesting active winds from the north-northwest at the time (midday) of the abrasion operations. Characteristics of some rocks, such as a two-toned appearance, suggest that they were possibly buried and exhumed on the order of 5 to 60 centimeters by wind deflation, depending on location.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Greeley, R -- Squyres, S W -- Arvidson, R E -- Bartlett, P -- Bell, J F 3rd -- Blaney, D -- Cabrol, N A -- Farmer, J -- Farrand, B -- Golombek, M P -- Gorevan, S P -- Grant, J A -- Haldemann, A F C -- Herkenhoff, K E -- Johnson, J -- Landis, G -- Madsen, M B -- McLennan, S M -- Moersch, J -- Rice, J W Jr -- Richter, L -- Ruff, S -- Sullivan, R J -- Thompson, S D -- Wang, A -- Weitz, C M -- Whelley, P -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):810-3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Box 871404, Tempe, AZ 85287-1404, USA. Greeley@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297660" target="_blank"〉PubMed〈/a〉
    Keywords: Evolution, Planetary ; Extraterrestrial Environment ; *Mars ; Wind
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  • 10
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    Surficial deposits at Gusev Crater along Spirit Rover traverses (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Mars Exploration Rover Spirit has traversed a fairly flat, rock-strewn terrain whose surface is shaped primarily by impact events, although some of the landscape has been altered by eolian processes. Impacts ejected basaltic rocks that probably were part of locally formed lava flows from at least 10 meters depth. Some rocks have been textured and/or partially buried by windblown sediments less than 2 millimeters in diameter that concentrate within shallow, partially filled, circular impact depressions referred to as hollows. The terrain traversed during the 90-sol (martian solar day) nominal mission shows no evidence for an ancient lake in Gusev crater.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Grant, J A -- Arvidson, R -- Bell, J F 3rd -- Cabrol, N A -- Carr, M H -- Christensen, P -- Crumpler, L -- Des Marais, D J -- Ehlmann, B L -- Farmer, J -- Golombek, M -- Grant, F D -- Greeley, R -- Herkenhoff, K -- Li, R -- McSween, H Y -- Ming, D W -- Moersch, J -- Rice, J W Jr -- Ruff, S -- Richter, L -- Squyres, S -- Sullivan, R -- Weitz, C -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):807-10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA. grantj@nasm.si.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297659" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geologic Sediments ; *Mars ; Minerals ; Silicates ; Volcanic Eruptions ; 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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