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NARROW
GeoRef Subject
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all geography including DSDP/ODP Sites and Legs
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Asia
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Chukotka Russian Federation (1)
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Kamchatka Russian Federation
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Kamchatka Peninsula (1)
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Magadan Russian Federation (1)
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Canada
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Eastern Canada
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Quebec
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Oka Complex (1)
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Commonwealth of Independent States
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Russian Federation
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Chukotka Russian Federation (1)
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Kamchatka Russian Federation
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Kamchatka Peninsula (1)
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Magadan Russian Federation (1)
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East Pacific Ocean Islands
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Hawaii
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Hawaii County Hawaii
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Hawaii Island
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Halemaumau Crater (1)
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Kilauea (2)
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Mauna Kea (1)
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Mauna Loa (1)
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Europe
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Southern Europe
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Italy
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Sicily Italy
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Mount Etna (1)
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Oceania
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Polynesia
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Hawaii
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Hawaii County Hawaii
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Hawaii Island
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Halemaumau Crater (1)
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Kilauea (2)
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Mauna Loa (1)
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United States
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Columbia Plateau (1)
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Hawaii
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Hawaii County Hawaii
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Halemaumau Crater (1)
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Kilauea (2)
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Mauna Kea (1)
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Mauna Loa (1)
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commodities
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metal ores
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copper ores (1)
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iron ores (1)
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mineral deposits, genesis (1)
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mineral exploration (1)
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mineral resources (1)
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elements, isotopes
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carbon (1)
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chemical elements (1)
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Ar-38/Ar-36 (1)
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stable isotopes
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Ar-38/Ar-36 (1)
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He-4/He-3 (1)
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metals
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actinides
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alkali metals
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noble gases
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argon
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helium
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He-4/He-3 (1)
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krypton
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Kr-84 (1)
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neon
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xenon
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geologic age
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Phanerozoic (1)
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Precambrian
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upper Precambrian
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igneous rocks
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igneous rocks
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carbonatites (1)
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volcanic rocks
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basalts
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glasses (1)
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ophiolite (1)
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Primary terms
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Asia
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pallasite (1)
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stony meteorites
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achondrites
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HED meteorites (1)
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chassignite
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Chassigny Meteorite (1)
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nakhlite
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Nakhla Meteorite (1)
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shergottite
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chondrites
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neon
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xenon
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Oceania
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Polynesia
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Hawaii
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Halemaumau Crater (1)
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Venus
The Quest for Extraterrestrial Cratons
Characterizing basalt-atmosphere interactions on Venus: A review of thermodynamic and experimental results
Tesserae: Surface differences across Venus’s “continents”
Galaxy of Green
Mitigating Power and Memory Constraints on a Venusian Seismometer
An overview of GPR subsurface exploration of planets and moons
Mars as a time machine to Precambrian Earth
Water in Differentiated Planets, the Moon, and Asteroids
The Air Over There: Exploring Exoplanet Atmospheres
Precambrian tectonic evolution of Earth: an outline
Venus, An Active Planet: Evidence for Recent Volcanic and Tectonic Activity
Venus tesserae feature layered, folded, and eroded rocks
Redox Processes in Early Earth Accretion and in Terrestrial Bodies
U, Th, and K partitioning between metal, silicate, and sulfide and implications for Mercury's structure, volatile content, and radioactive heat production
Principles of structural geology on rocky planets
ABSTRACT Small shield volcanoes with basal diameters <20 km represent the most abundant type of volcano on Venus. These shield volcanoes number >>10 6 in population and often occur in clusters known as shield fields, which have been interpreted to be analogous to basaltic volcanic fields on Earth. Despite previous work on shield fields, questions related to edifice morphology and magma viscosity, timing relations of events across an individual field, volume of erupted material, and the role of tectonic structures are still unresolved. Here, we address those questions through geologic mapping, volumetric calculations, and statistical analysis of possible edifice alignments in six venusian shield fields: Asherat Colles, Chernava Colles, Monoshi Tholus, Nordenflycht Patera, Ran Colles, and Urutonga Colles. Our results indicate that all of these shield fields and their associated deposits are younger than the surrounding units within the mapping areas, and each field displays overlapping temporal relations with local extensional and contractional structures. Each field also displays a lack of a consistent pattern in the temporal distribution of volcanism with regards to edifice type. Analyses of possible edifice alignments suggest edifice trends that are consistent with mapped tectonic structures within all studied fields except Asherat Colles. Comparison of these six venusian fields to terrestrial basaltic volcanic fields shows that venusian fields may be up to two to three orders of magnitude larger in their areal expanse and volume of erupted material. Our results are consistent with previous interpretations of venusian shield fields representing low rates (likely <5 × 10 −4 km 3 /yr) of magma supply feeding these magmatic centers and highlight the effects of the resolution limit of the Magellan data set on interpreting fundamental geologic processes on the venusian surface.