Geology and structure of Beta Regio, Venus: Results from Arecibo Radar Imaging
Arecibo radar images of a portion of the equatorial region of Venus provide the first high resolution (1.5- to 2.0-km) synoptic coverage of Beta Regio. Within this area, tessera, a complex deformed terrain, is identified as a major geologic unit with the largest region corresponding to a plateau on...
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| Veröffentlicht in: | Geophysical research letters 1991-06, Vol.18 (6), p.1159-1162 |
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| container_title | Geophysical research letters |
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| creator | Senske, D. A. Head, J. W. Stofan, E. R. Campbell, D. B. |
| description | Arecibo radar images of a portion of the equatorial region of Venus provide the first high resolution (1.5- to 2.0-km) synoptic coverage of Beta Regio. Within this area, tessera, a complex deformed terrain, is identified as a major geologic unit with the largest region corresponding to a plateau on the east flank of the highland. Three models are proposed to explain the origin and evolution of Beta Regio and are identified as Mantle Plume/Passive Crust, Mantle Plume/Active Crust, and Mantle Plume/Crustal Spreading. The Mantle Plume/Passive Crust model appears to be the most consistent with the geology in this region and suggests that a plume disrupts a preexisting region of tessera. |
| doi_str_mv | 10.1029/91GL01001 |
| format | Article |
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A.</creatorcontrib><creatorcontrib>Head, J. W.</creatorcontrib><creatorcontrib>Stofan, E. R.</creatorcontrib><creatorcontrib>Campbell, D. B.</creatorcontrib><title>Geology and structure of Beta Regio, Venus: Results from Arecibo Radar Imaging</title><title>Geophysical research letters</title><addtitle>Geophys. Res. Lett</addtitle><description>Arecibo radar images of a portion of the equatorial region of Venus provide the first high resolution (1.5- to 2.0-km) synoptic coverage of Beta Regio. Within this area, tessera, a complex deformed terrain, is identified as a major geologic unit with the largest region corresponding to a plateau on the east flank of the highland. Three models are proposed to explain the origin and evolution of Beta Regio and are identified as Mantle Plume/Passive Crust, Mantle Plume/Active Crust, and Mantle Plume/Crustal Spreading. The Mantle Plume/Passive Crust model appears to be the most consistent with the geology in this region and suggests that a plume disrupts a preexisting region of tessera.</description><subject>640107 - Astrophysics & Cosmology- Planetary Phenomena</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>DATA</subject><subject>DATA ANALYSIS</subject><subject>GEOLOGY</subject><subject>INFORMATION</subject><subject>Lunar And Planetary Exploration</subject><subject>MATHEMATICAL MODELS</subject><subject>MEASURING INSTRUMENTS</subject><subject>ORIGIN</subject><subject>PLANETARY EVOLUTION</subject><subject>PLANETS</subject><subject>RADAR</subject><subject>RANGE FINDERS</subject><subject>RESOLUTION</subject><subject>SOLAR SYSTEM EVOLUTION</subject><subject>TOPOGRAPHY</subject><subject>VENUS PLANET</subject><issn>0094-8276</issn><issn>1944-8007</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1991</creationdate><recordtype>article</recordtype><sourceid>CYI</sourceid><recordid>eNp9kUtv1DAQgC0EUpfCoXcOFgcEUrfY8Svm1l3RULEq0qrQo-U4k8WQjYvtCPbf41Wq3uAyz28emkHojJILSir9XtNmQygh9AlaUM35siZEPUULQnSxKyVP0POUfhBCGGF0gW4aCEPYHbAdO5xynFyeIuDQ4xVki7ew8-Ecf4NxSh-Kl6YhJ9zHsMeXEZxvA97azkZ8vbc7P-5eoGe9HRK8fNCn6OvVx9v1p-XmS3O9vtwsLWdlEd7XIFstme3BaqiLUKqVuheCMtaSjjnR60prylvWdW0JK9G3shbcUdA1O0Wv574hZW-S8xncdxfGEVw2glHJ5RF6M0P3MfyaIGWz98nBMNgRwpRMJapKVkoX8O1_QSqqsrasOC3ouxl1MaQUoTf30e9tPBhKzPED5vEDhb2Y2d9-gMO_QdNsN4IrXgpezQWjTdaMOZbR5QaECFGzY3o5p33K8Oexn40_jVRMCXN305ir27v1inxeGcX-AqRDmwo</recordid><startdate>199106</startdate><enddate>199106</enddate><creator>Senske, D. 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B.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a4394-4f8e6b963afea9e8ea977b69f55133b0d3c5f929914b3ddb55175fb6854c1e983</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1991</creationdate><topic>640107 - Astrophysics & Cosmology- Planetary Phenomena</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>DATA</topic><topic>DATA ANALYSIS</topic><topic>GEOLOGY</topic><topic>INFORMATION</topic><topic>Lunar And Planetary Exploration</topic><topic>MATHEMATICAL MODELS</topic><topic>MEASURING INSTRUMENTS</topic><topic>ORIGIN</topic><topic>PLANETARY EVOLUTION</topic><topic>PLANETS</topic><topic>RADAR</topic><topic>RANGE FINDERS</topic><topic>RESOLUTION</topic><topic>SOLAR SYSTEM EVOLUTION</topic><topic>TOPOGRAPHY</topic><topic>VENUS PLANET</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Senske, D. A.</creatorcontrib><creatorcontrib>Head, J. W.</creatorcontrib><creatorcontrib>Stofan, E. R.</creatorcontrib><creatorcontrib>Campbell, D. B.</creatorcontrib><collection>Istex</collection><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>Geophysical research letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Senske, D. A.</au><au>Head, J. W.</au><au>Stofan, E. R.</au><au>Campbell, D. B.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Geology and structure of Beta Regio, Venus: Results from Arecibo Radar Imaging</atitle><jtitle>Geophysical research letters</jtitle><addtitle>Geophys. Res. Lett</addtitle><date>1991-06</date><risdate>1991</risdate><volume>18</volume><issue>6</issue><spage>1159</spage><epage>1162</epage><pages>1159-1162</pages><issn>0094-8276</issn><eissn>1944-8007</eissn><abstract>Arecibo radar images of a portion of the equatorial region of Venus provide the first high resolution (1.5- to 2.0-km) synoptic coverage of Beta Regio. Within this area, tessera, a complex deformed terrain, is identified as a major geologic unit with the largest region corresponding to a plateau on the east flank of the highland. Three models are proposed to explain the origin and evolution of Beta Regio and are identified as Mantle Plume/Passive Crust, Mantle Plume/Active Crust, and Mantle Plume/Crustal Spreading. The Mantle Plume/Passive Crust model appears to be the most consistent with the geology in this region and suggests that a plume disrupts a preexisting region of tessera.</abstract><cop>Legacy CDMS</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/91GL01001</doi><tpages>4</tpages></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0094-8276 |
| ispartof | Geophysical research letters, 1991-06, Vol.18 (6), p.1159-1162 |
| issn | 0094-8276 1944-8007 |
| language | eng |
| recordid | cdi_osti_scitechconnect_5316468 |
| source | Wiley Online Library Journals Frontfile Complete; NASA Technical Reports Server |
| subjects | 640107 - Astrophysics & Cosmology- Planetary Phenomena CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS DATA DATA ANALYSIS GEOLOGY INFORMATION Lunar And Planetary Exploration MATHEMATICAL MODELS MEASURING INSTRUMENTS ORIGIN PLANETARY EVOLUTION PLANETS RADAR RANGE FINDERS RESOLUTION SOLAR SYSTEM EVOLUTION TOPOGRAPHY VENUS PLANET |
| title | Geology and structure of Beta Regio, Venus: Results from Arecibo Radar Imaging |
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