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  • 1
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    Venus southern hemisphere: geologic character and age of terrains in the themis-alpha-lada region (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-01-11
    Description: Arecibo high-resolution radar images of the southern hemisphere of Venus extending to 78 degrees S show that the surface of the Themis-Alpha-Lada region is characterized by linear deformation zones with volcanoes and corona-like features and by regional volcanic deposits (primarily plains, small shields, and large edifices). Large-scale areal deformation is limited to the tessera of Alpha Regio. Lada Terra, in the southern high latitudes, contains several large coronae, in contrast to Ishtar Terra in the northern high latitudes. The density of craters of possible impact origin is somewhat lower than that observed in the Venera 15 and 16 coverage; these data extend to 43 percent of the areas of the surface of Venus with ages of less than about 1 billion years.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Campbell, D B -- Senske, D A -- Head, J W -- Hine, A A -- Fisher, P C -- New York, N.Y. -- Science. 1991 Jan 11;251(4990):180-3.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17836947" 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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  • 2
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    Venus tectonics: initial analysis from magellan (1991)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1991-04-12
    Description: Radar imaging and altimetry data from the Magellan mission have revealed a diversity of deformational features at a variety of spatial scales on the Venus surface. The plains record a superposition of different episodes of deformation and volcanism; strain is both areally distributed and concentrated into zones of extension and shortening. The common coherence of strain patterns over hundreds of kilometers implies that many features in the plains reflect a crustal response to mantle dynamic processes. Ridge belts and mountain belts represent successive degrees of lithospheric shortening and crustal thickening; the mountain belts also show widespread evidence for extension and collapse both during and following crustal compression. Venus displays two geometrical patterns of concentrated lithospheric extension: quasi-circular coronae and broad rises with linear rift zones; both are sites of significant volcanism. No long, large-offset strike-slip faults have been observed, although limited local horizontal shear is accommodated across many zones of crustal shortening. In general, tectonic features on Venus are unlike those in Earth's oceanic regions in that strain typically is distributed across broad zones that are one to a few hundred kilometers wide, and separated by stronger and less deformed blocks hundreds of kilometers in width, as in actively deforming continental regions on Earth.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Solomon, S C -- Head, J W -- Kaula, W M -- McKenzie, D -- Parsons, B -- Phillips, R J -- Schubert, G -- Talwani, M -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):297-312.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769277" target="_blank"〉PubMed〈/a〉
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  • 3
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    Venus volcanism: initial analysis from magellan data (1991)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1991-04-12
    Description: Magellan images confirm that volcanism is widespread and has been fimdamentally important in the formation and evolution of the crust of Venus. High-resolution imaging data reveal evidence for intrusion (dike formation and cryptodomes) and extrusion (a wide range of lava flows). Also observed are thousands of small shield volcanoes, larger edifices up to several hundred kilometers in diameter, massive outpourings of lavas, and local pyroclastic deposits. Although most features are consistent with basaltic compositions, a number of large pancake-like domes are morphologically similar to rhyolite-dacite domes on Earth. Flows and sinuous channels with lengths of many hundreds of kilometers suggest that extremely high effusion rates or very fluid magmas (perhaps komatiites) may be present. Volcanism is evident in various tectonic settings (coronae, linear extensional and compressional zones, mountain belts, upland rises, highland plateaus, and tesserae). Volcanic resurfacing rates appear to be low (less than 2 Km(3)/yr) but the significance of dike formation and intrusions, and the mode of crustal formation and loss remain to be established.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Head, J W -- Campbell, D B -- Elachi, C -- Guest, J E -- McKenzie, D P -- Saunders, R S -- Schaber, G G -- Schubert, G -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):276-88.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769275" target="_blank"〉PubMed〈/a〉
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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〉
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  • 5
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    An overview of venus geology (1991)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1991-04-12
    Description: The Magellan spacecraft is producing comprehensive image and altimetry data for the planet Venus. Initial geologic mapping of the planet reveals a surface dominated by volcanic plains and characterized by extensive volcanism and tectonic deformation. Geologic and geomorphologic units include plains terrains, tectonic terrains, and surficial material units. Understanding the origin of these units and the relation between them is an ongoing task of the Magellan team.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Saunders, R S -- Arvidson, R E -- Head, J W 3rd -- Schaber, G G -- Stofan, E R -- Solomon, S C -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):249-52.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769270" target="_blank"〉PubMed〈/a〉
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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)
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    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〉
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  • 7
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    Fundamental issues in the geology and geophysics of venus (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-04-12
    Description: A number of important and currently unresolved issues in the global geology and geophysics of Venus will be addressable with the radar imaging, altimetry, and gravity measurements now forthcoming from the Magellan mission. Among these are the global volcanic flux and the rate of formation of new crust; the global heat flux and its regional variations; the relative importance of localized hot spots and linear centers of crustal spreading to crustal formation and tectonics; and the planform of mantle convection on Venus and the nature of the interactions among interior convective flow, near-surface deformation and magmatism.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Solomon, S C -- Head, J W -- New York, N.Y. -- Science. 1991 Apr 12;252(5003):252-60.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17769271" target="_blank"〉PubMed〈/a〉
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  • 8
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    First images of asteroid 243 ida (1994)
    American Association for the Advancement of Science (AAAS)
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    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〉
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  • 9
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    Relation of major volcanic center concentration on venus to global tectonic patterns (1993)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1993-07-30
    Description: Global analysis of NASA Magellan image data indicates that a major concentration of volcanic centers covering approximately 40 percent of the surface of Venus occurs between the Beta, Atla, and Themis regiones. Associated with this enhanced concentration are geological characteristics commonly interpreted as rifting and mantle upwelling. Interconnected low plains in an annulus around this concentration are characterized by crustal shortening and infrequent volcanic centers that may represent sites of mantle return flow and net down-welling. Together, these observations suggest the existence of relatively simple, largescale patterns of mantle circulation similar to those associated with concentrations of intraplate volcanism on Earth.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Crumpler, L S -- Head, J W -- Aubele, J C -- New York, N.Y. -- Science. 1993 Jul 30;261(5121):591-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17758169" target="_blank"〉PubMed〈/a〉
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  • 10
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    Galileo multispectral imaging of the north polar and eastern limb regions of the moon (1994)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1994-05-20
    Description: Multispectral images obtained during the Galileo probe's second encounter with the moon reveal the compositional nature of the north polar regions and the northeastern limb. Mare deposits in these regions are found to be primarily low to medium titanium lavas and, as on the western limb, show only slight spectral heterogeneity. The northern light plains are found to have the spectral characteristics of highlands materials, show little evidence for the presence of cryptomaria, and were most likely emplaced by impact processes regardless of their age.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Belton, M J -- Greeley, R -- Greenberg, R -- Geissler, P -- McEwen, A -- Klaasen, K P -- Heffernan, C -- Breneman, H -- Johnson, T V -- Head, J W 3rd -- Pieters, C -- Neukum, G -- Chapman, C R -- Anger, C -- Carr, M H -- Davies, M E -- Fanale, F P -- Gierasch, P J -- Thompson, W R -- Veverka, J -- Sagan, C -- Ingersoll, A P -- Pilcher, C B -- New York, N.Y. -- Science. 1994 May 20;264(5162):1112-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17744892" target="_blank"〉PubMed〈/a〉
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