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RESEARCH PAPER · Icarus · 2016

Venus’ radar-bright highlands: Different signatures and materials on Ovda Regio and on Maxwell Montes

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Venus’ radar-bright highlands: Different signatures and materials on Ovda Regio and on Maxwell MontesOriginalVenus Surface Composition Constrained by Observation and Experiment128Water and Volatile Inventories of Mercury, Venus, the Moon, and Mars0Surface properties and surficial deposits on Venus: New results from Magellan radar altimeter data analysis14Water and Volatile Inventories of Mercury, Venus, the Moon, and Mars40Gas–Solid Interactions on Venus and Other Solar System Bodies57Ovda Fluctus, the Festoon Lava Flow on Ovda Regio, Venus: Not Silica‐Rich25Investigation into the radar anomaly on Venus: The effect of Venus conditions on bismuth, tellurium, and sulfur mixtures15Solar System Radio Astronomy0Low radar emissivity signatures on Venus volcanoes and coronae: New insights on relative composition and age47Venus: A phase equilibria approach to model surface alteration as a function of rock composition, oxygen- and sulfur fugacities28Variations in the radiophysical properties of tesserae and mountain belts on Venus: Classification and mineralogical trends15Distinct Mineralogy and Age of Individual Lava Flows in Atla Regio, Venus Derived From Magellan Radar Emissivity31Near-infrared Reflectance of Rocks at High Temperature: Preliminary Results and Implications for Near-infrared Emissivity of Venus’s Surface11Laboratory Studies in Support of Venus Exploration: Surface and Near-Surface1Phosphine on Venus Cannot Be Explained by Conventional Processes68Phosphorus in the Clouds of Venus: Potential for Bioavailability21Thermochemical Equilibrium Modeling Indicates That Hg Minerals Are Unlikely to Be the Source of the Emissivity Signal on the Highlands of Venus2Radiative Transfer Simulations for the Observed Decrease of Radio Brightness Temperature of Venus With Increasing Decimeter Wavelengths: Possible Existence of a Reflective or Quasi‐Conductive Subsurface2Extended Rift‐Associated Volcanism in Ganis Chasma, Venus Detected From Magellan Radar Emissivity17Experiments on the reactivity of basaltic minerals and glasses in Venus surface conditions using the Glenn Extreme Environment Rig19The Venus Emissivity Mapper: implementation for flight on the NASA VERITAS mission7The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere5Exploring Venus subsurface: Analysis of geological targets and their properties5Experimental Weathering of Rocks and Minerals at Venus Conditions in the Glenn Extreme Environments Rig (GEER)18Microwaving Mimas, Enceladus, Tethys, Dione, Rhea, Iapetus and Phoebe: Insights into the regolith properties and geological history of Saturn's icy satellites8Characterizing basalt-atmosphere interactions on Venus: A review of thermodynamic and experimental results9Mineralogy of the Venus Surface23Dyke swarm history in Belet-ili and Gaia (Gaya) Coronae Region (13°–26°E, 0°–10°N), Central Eistla Regio, Venus8Planetary Radar—State-of-the-Art Review17Far-travelled 3700 km lateral magma propagation just below the surface of Venus15Heng-o Corona, Venus: Dyke swarms record evolution of its underlying mantle plume8Volcanic and Tectonic Constraints on the Evolution of Venus25Graben systems and geological history of Mbokomu Mons region, Parga Chasmata, Venus3Dyke swarms of Onenhste and adjacent coronae in Parga Chasmata, SE of Atla Regio, Venus: Detailed mapping, swarm interactions and geological history5Venus2Radar Anomaly (Venus)0Geological history of Theia Mons, Beta Regio plume, Venus: Recognition of two main magmatic centers for flows, radiating dyke swarms and triple junction rifting3Geological history of Samodiva Mons shield volcano, and surrounding area, Quadrangle V-29, Venus2Microwave Emissivity Variations Across Ovda Regio, Venus1Assessing the evidence for active volcanism on Venus: current limitations and prospects for future investigations11The Effect of Near‐Surface Winds on Surface Temperature and Dust Transport on Venus2Dyke swarm history of the northeastern margin of Central Ovda Regio, Venus: Evidence for mantle plume arrival and triple junction rifting0Oxygen fugacity as a control on Venusian basalt mineralogy: Constraints from experiments and thermodynamic modeling0Intra‐Tessera Plains: Implications of Their Radar Properties for Surface Processes on Venus0

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  2. Water and Volatile Inventories of Mercury, Venus, the Moon, and Mars

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  5. Gas–Solid Interactions on Venus and Other Solar System Bodies

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  6. Ovda Fluctus, the Festoon Lava Flow on Ovda Regio, Venus: Not Silica‐Rich

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  7. Investigation into the radar anomaly on Venus: The effect of Venus conditions on bismuth, tellurium, and sulfur mixtures

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    S. T. Port, V. F. Chevrier, Erika Köhler

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  8. Solar System Radio Astronomy

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  9. Low radar emissivity signatures on Venus volcanoes and coronae: New insights on relative composition and age

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  10. Venus: A phase equilibria approach to model surface alteration as a function of rock composition, oxygen- and sulfur fugacities

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  11. Variations in the radiophysical properties of tesserae and mountain belts on Venus: Classification and mineralogical trends

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  12. Distinct Mineralogy and Age of Individual Lava Flows in Atla Regio, Venus Derived From Magellan Radar Emissivity

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  13. Near-infrared Reflectance of Rocks at High Temperature: Preliminary Results and Implications for Near-infrared Emissivity of Venus’s Surface

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  14. Laboratory Studies in Support of Venus Exploration: Surface and Near-Surface

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  18. Radiative Transfer Simulations for the Observed Decrease of Radio Brightness Temperature of Venus With Increasing Decimeter Wavelengths: Possible Existence of a Reflective or Quasi‐Conductive Subsurface

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  19. Extended Rift‐Associated Volcanism in Ganis Chasma, Venus Detected From Magellan Radar Emissivity

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  22. The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere

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  23. Exploring Venus subsurface: Analysis of geological targets and their properties

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  24. Experimental Weathering of Rocks and Minerals at Venus Conditions in the Glenn Extreme Environments Rig (GEER)

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