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  • 1
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    Martian surface/near-surface water inventory: Sources, sinks, and changes with time. (2015)
    Wiley
    Details
    Publication Date: 2015-01-13
    Description: Today a 34 m global equivalent water layer (GEL) lies in the martian polar layered deposits and shallow ground ice. During the Amazonian 3 m was outgassed and 31 m was lost to space and to the surface, leaving 62 m at the end of Hesperian. During the Hesperian, volcanic outgassing added 5 m, 7 m was lost and 40 m GEL of groundwater was added to form outflow channels, leaving 24 m carry-over of surface water from the Noachian into the Hesperian. The Hesperian budget is incompatible with a northern ocean during this era. These figures are for near-surface water; substantial amounts of water may have existed as deep ground ice and groundwater. Our estimate of approximately 24 m near-surface water in the Late Noachian, is insufficient to support an ocean at that time also and favors episodic melting of an icy highlands to produce the fluvial and lacustrine features.
    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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  • 2
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    Early views of the martian surface from the Mars Orbiter Camera of Mars Global Surveyor (1998)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1998-03-28
    Description: High-resolution images of the martian surface at scales of a few meters show ubiquitous erosional and depositional eolian landforms. Dunes, sandsheets, and drifts are prevalent and exhibit a range of morphology, composition (inferred from albedo), and age (as seen in occurrences of different dune orientations at the same location). Steep walls of topographic depressions such as canyons, valleys, and impact craters show the martian crust to be stratified at scales of a few tens of meters. The south polar layered terrain and superposed permanent ice cap display diverse surface textures that may reflect the complex interplay of volatile and non-volatile components. Low resolution regional views of the planet provide synoptic observations of polar cap retreat, condensate clouds, and the lifecycle of local and regional dust storms.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Malin, M C -- Carr, M H -- Danielson, G E -- Davies, M E -- Hartmann, W K -- Ingersoll, A P -- James, P B -- Masursky, H -- McEwen, A S -- Soderblom, L A -- Thomas, P -- Veverka, J -- Caplinger, M A -- Ravine, M A -- Soulanille, T A -- Warren, J L -- New York, N.Y. -- Science. 1998 Mar 13;279(5357):1681-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Malin Space Science Systems, Post Office Box 910148, San Diego, CA 92191-0148, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9497280" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Dioxide ; *Extraterrestrial Environment ; Ice ; *Mars ; Spacecraft
    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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    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
    Published by American Association for the Advancement of Science (AAAS)
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  • 4
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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 5
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    High-temperature silicate volcanism on Jupiter's moon Io (1998)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1998-07-04
    Description: Infrared wavelength observations of Io by the Galileo spacecraft show that at least 12 different vents are erupting lavas that are probably hotter than the highest temperature basaltic eruptions on Earth today. In at least one case, the eruption near Pillan Patera, two independent instruments on Galileo show that the lava temperature must have exceeded 1700 kelvin and may have reached 2000 kelvin. The most likely explanation is that these lavas are ultramafic (magnesium-rich) silicates, and this idea is supported by the tentative identification of magnesium-rich orthopyroxene in lava flows associated with these high-temperature hot spots.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McEwen, A S -- Keszthelyi, L -- Spencer, J R -- Schubert, G -- Matson, D L -- Lopes-Gautier, R -- Klaasen, K P -- Johnson, T V -- Head, J W -- Geissler, P -- Fagents, S -- Davies, A G -- Carr, M H -- Breneman, H H -- Belton, M J -- New York, N.Y. -- Science. 1998 Jul 3;281(5373):87-90.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85711, USA. mcewen@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9651251" target="_blank"〉PubMed〈/a〉
    Keywords: *Extraterrestrial Environment ; Hot Temperature ; *Jupiter ; Minerals ; *Silicates ; 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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  • 6
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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 7
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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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  • 8
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    The Opportunity Rover's Athena science investigation at Meridiani Planum, Mars (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-12-04
    Description: The Mars Exploration Rover Opportunity has investigated the landing site in Eagle crater and the nearby plains within Meridiani Planum. The soils consist of fine-grained basaltic sand and a surface lag of hematite-rich spherules, spherule fragments, and other granules. Wind ripples are common. Underlying the thin soil layer, and exposed within small impact craters and troughs, are flat-lying sedimentary rocks. These rocks are finely laminated, are rich in sulfur, and contain abundant sulfate salts. Small-scale cross-lamination in some locations provides evidence for deposition in flowing liquid water. We interpret the rocks to be a mixture of chemical and siliciclastic sediments formed by episodic inundation by shallow surface water, followed by evaporation, exposure, and desiccation. Hematite-rich spherules are embedded in the rock and eroding from them. We interpret these spherules to be concretions formed by postdepositional diagenesis, again involving liquid water.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Squyres, S W -- Arvidson, R E -- Bell, J F 3rd -- Bruckner, J -- Cabrol, N A -- Calvin, W -- Carr, M H -- Christensen, P R -- Clark, B C -- Crumpler, L -- Marais, D J Des -- d'Uston, C -- Economou, T -- Farmer, J -- Farrand, W -- Folkner, W -- Golombek, M -- Gorevan, S -- Grant, J A -- Greeley, R -- Grotzinger, J -- Haskin, L -- Herkenhoff, K E -- Hviid, S -- Johnson, J -- Klingelhofer, G -- Knoll, A H -- Landis, G -- Lemmon, M -- Li, R -- Madsen, M B -- Malin, M C -- McLennan, S M -- McSween, H Y -- Ming, D W -- Moersch, J -- Morris, R V -- Parker, T -- Rice, J W Jr -- Richter, L -- Rieder, R -- Sims, M -- Smith, M -- Smith, P -- Soderblom, L A -- Sullivan, R -- Wanke, H -- Wdowiak, T -- Wolff, M -- Yen, A -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1698-703.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. squyres@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576602" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Evolution, Planetary ; Extraterrestrial Environment ; Ferric Compounds ; Geologic Sediments ; *Mars ; Minerals ; Silicates ; Spacecraft ; Water ; Wind
    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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    The Spirit Rover's Athena science investigation at Gusev Crater, Mars (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Mars Exploration Rover Spirit and its Athena science payload have been used to investigate a landing site in Gusev crater. Gusev is hypothesized to be the site of a former lake, but no clear evidence for lacustrine sedimentation has been found to date. Instead, the dominant lithology is basalt, and the dominant geologic processes are impact events and eolian transport. Many rocks exhibit coatings and other characteristics that may be evidence for minor aqueous alteration. Any lacustrine sediments that may exist at this location within Gusev apparently have been buried by lavas that have undergone subsequent impact disruption.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Squyres, S W -- Arvidson, R E -- Bell, J F 3rd -- Bruckner, J -- Cabrol, N A -- Calvin, W -- Carr, M H -- Christensen, P R -- Clark, B C -- Crumpler, L -- Des Marais, D J -- D'Uston, C -- Economou, T -- Farmer, J -- Farrand, W -- Folkner, W -- Golombek, M -- Gorevan, S -- Grant, J A -- Greeley, R -- Grotzinger, J -- Haskin, L -- Herkenhoff, K E -- Hviid, S -- Johnson, J -- Klingelhofer, G -- Knoll, A -- Landis, G -- Lemmon, M -- Li, R -- Madsen, M B -- Malin, M C -- McLennan, S M -- McSween, H Y -- Ming, D W -- Moersch, J -- Morris, R V -- Parker, T -- Rice, J W Jr -- Richter, L -- Rieder, R -- Sims, M -- Smith, M -- Smith, P -- Soderblom, L A -- Sullivan, R -- Wanke, H -- Wdowiak, T -- Wolff, M -- Yen, A -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):794-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Cornell University, Ithaca, NY 14853, USA. squyres@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297657" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; Geologic Sediments ; Geological Phenomena ; Geology ; Magnetics ; *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
    Published by American Association for the Advancement of Science (AAAS)
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  • 10
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    First images of asteroid 243 ida (1994)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1994-09-09
    Description: The first images of the asteroid 243 Ida from Galileo show an irregular object measuring 56-kilometers by 24 kilometers by 21 kilometers. Its surface is rich in geologic features, including systems of grooves, blocks, chutes, albedo features, crater chains, and a full range of crater morphologies. The largest blocks may be distributed nonuniformly across the surface; lineaments and dark-floored craters also have preferential locations. Ida is interpreted to have a substantial regolith. The high crater density and size-frequency distribution (-3 differential power-law index) indicate a surface in equilibrium with saturated cratering. A minimum model crater age for Ida-and therefore for the Koronis family to which Ida belongs-is estimated at 1 billion years, older than expected.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Belton, M J -- Chapman, C R -- Veverka, J -- Klaasen, K P -- Harch, A -- Greeley, R -- Greenberg, R -- Head, J W 3rd -- McEwen, A -- Morrison, D -- Thomas, P C -- Davies, M E -- Carr, M H -- Neukum, G -- Fanale, F P -- Davis, D R -- Anger, C -- Gierasch, P J -- Ingersoll, A P -- Pilcher, C B -- New York, N.Y. -- Science. 1994 Sep 9;265(5178):1543-7.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17801529" 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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