Venus tectonics: An overview of Magellan observations

@article{Solomon1992VenusTA,
  title={Venus tectonics: An overview of Magellan observations},
  author={S. Solomon and S. Smrekar and D. Bindschadler and R. Grimm and W. M. Kaula and G. Mcgill and R. Phillips and R. Saunders and G. Schubert and S. Squyres and E. Stofan},
  journal={Journal of Geophysical Research},
  year={1992},
  volume={97},
  pages={13199-13255}
}
The nearly global radar imaging and altimetry measurements of the surface of Venus obtained by the Magellan spacecraft have revealed that deformational features of a wide variety of styles and spatial scales are nearly ubiquitous on the planet. Many areas of Venus record a superposition of different episodes of deformation and volcanism. This deformation is manifested both in areally distributed strain of modest magnitude, such as families of graben and wrinkle ridges at a few to a few tens of… Expand
Plains tectonism on Venus: The deformation belts of Lavinia Planitia
High-resolution radar images from the Magellan spacecraft have revealed the first details of the morphology of the Lavinia Planitia region of Venus. A number of geologic units can be distinguished,Expand
Gravitational Spreading of High Terrain in Ishtar Terra, Venus
Magellan altimetry measurements indicate that the mountain belts and plateau margins of Ishtar Terra have topographic slopes in the range 2–30°. Magellan radar images reveal that numerous sets ofExpand
The tectonics of Venus
  • W. M. Kaula
  • Geology
  • Philosophical Transactions of the Royal Society of London. Series A: Physical and Engineering Sciences
  • 1994
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Styles of deformation in Ishtar Terra and their implications
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An episodic hypothesis for Venusian tectonics
It is suggested that episodic plate tectonics occurs on Venus; episodes of rapid plate tectonics are separated by periods of surface quiescence. For the last 500 ± 200 m.y. it is postulated that theExpand
Tectonic evolution of Bell Regio, Venus: lithospheric flexure, and edifice stresses
In order to understand the relationship between volcanic and tectonic processes and the stress state in the lithosphere of Venus, we analyzed the stress environments and resulting tectonic featuresExpand
Tectonic evolution of Bell Regio, Venus: Regional stress, lithospheric flexure, and edifice stresses
In order to understand the relationship between volcanic and tectonic processes and the stress state in the lithosphere of Venus, we analyzed the stress environments and resulting tectonic featuresExpand
A globally fragmented and mobile lithosphere on Venus
TLDR
A pattern of tectonic deformation on Venus is identified that suggests that many of the planet’s lowlands have fragmented into discrete crustal blocks, and that these blocks have moved relative to each other in the geologically recent past, suggesting a style of interior–surface coupling not seen elsewhere in the inner Solar System except for continental interiors on Earth. Expand
Coldspots and hotspots - Global tectonics and mantle dynamics of Venus
Magellan radar images and altimetry data and Pioneer Venus gravity data of major highlands and lowlands on Venus are examined with the objective of relating these tectonic and volcanic landforms toExpand
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References

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Venus Tectonics: Initial Analysis from Magellan
TLDR
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. Expand
Plains tectonism on Venus: The deformation belts of Lavinia Planitia
High-resolution radar images from the Magellan spacecraft have revealed the first details of the morphology of the Lavinia Planitia region of Venus. A number of geologic units can be distinguished,Expand
Constraints on the lithospheric structure of Venus from mechanical models and tectonic surface features
Radar images of the surface of Venus show numerous structures that are interpreted as having formed due to horizontal compression and extension of the lithosphere. Many of these features exhibitExpand
Gravitational Spreading of High Terrain in Ishtar Terra, Venus
Magellan altimetry measurements indicate that the mountain belts and plateau margins of Ishtar Terra have topographic slopes in the range 2–30°. Magellan radar images reveal that numerous sets ofExpand
Anatomy of a Venusian hot spot - Geology, gravity, and mantle dynamics of Eistla Regio
Eistla Regio is a series of broad swells, each up to a few thousand kilometers in diameter, in the equatorial highlands of Venus. It is characterized by strong positive free-air gravity anomalies,Expand
Venus Volcanism: Initial Analysis from Magellan Data
TLDR
Magellan images confirm that volcanism is widespread and has been fimdamentally important in the formation and evolution of the crust of Venus and reveals a number of large pancake-like domes are morphologically similar to rhyolite-dacite domes on Earth. Expand
Styles of deformation in Ishtar Terra and their implications
Ishtar Terra, the highest region on Venus, appears to have characteristics of both plume uplifts and convergent belts. Magellan imagery over longitudes 330°–30°E indicates a great variety of tectonicExpand
Geophysical models for the formation and evolution of coronae on Venus
Coronae are large circular features on Venus characterized by an annulus of concentric tectonic features, interior fracturing, volcanism, and generally upraised topography. They are suggested to formExpand
Coldspots and hotspots - Global tectonics and mantle dynamics of Venus
Magellan radar images and altimetry data and Pioneer Venus gravity data of major highlands and lowlands on Venus are examined with the objective of relating these tectonic and volcanic landforms toExpand
Venus: Limited extension and volcanism along zones of lithospheric weakness
Three global-scale zones of possible tectonic origin are described as occurring along broad, low rises within the Equatorial Highlands on Venus (lat 50° N. to 50° S., long 60° to 310°). The twoExpand
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