The surface of Venus

@article{Basilevsky2003TheSO,
  title={The surface of Venus},
  author={Alexander T. Basilevsky and James W. Head},
  journal={Reports on Progress in Physics},
  year={2003},
  volume={66},
  pages={1699-1734}
}
Venus is a planet that is similar to Earth in terms of some important planetary parameters (size, mass, position in the solar system, presence of atmosphere) and different in terms of other, equally important ones (absence of an intrinsic magnetic field, large atmospheric mass, carbon dioxide composition of the atmosphere, lack of water, very high surface pressure and temperature). The surface morphology of Venus is dominated by the signatures of basaltic volcanism and tectonic deformation… 
Numerical modelling of Venus’mantle: the role of cratons in lithospheric overturns
Despite its similarities in bulk properties to Earth, Venus portrays a fundamentally different mode of surface tectonics. Venus is currently known to be operating in stagnant lid mode of mantle
Dynamics of fault motion and the origin of contrasting tectonic style between Earth and Venus
TLDR
It is proposed that strong dynamic weakening in friction is a key factor leading to substantial dynamic weakening on Earth but not on Venus, leading to the contrasting tectonic styles between Earth and Venus.
Sedimentary Processes on Earth , Mars , Titan , and Venus
The atmospheres of solid planets exert a fundamental control on their surfaces. Interactions between atmospheric and geologic processes influence the morphology and composition of surfaces, and over
Continental crust formation on early Earth controlled by intrusive magmatism
TLDR
It is suggested that the pre-plate-tectonics Archean Earth operated globally in the Plutonic squishy lid regime rather than in an Io-like heat-pipe regime, which is thought to apply to the dynamics of Venus.
The history of tectonism on Venus: A stratigraphic analysis
Plumeless Venus has ancient impact-accretionary surface
Venus displays thousands of old circular structures, with topographic rims 5-2000 km in diameter, that have the morphology and cookie-cutter superposition required of impact craters and basins. Many
Volcanism and its role in Climate on Venus
There has clearly been significant volcanic activity on the surface of Venus in recent geological epochs and there is a great deal of indirect evidence that this may continue at the present time.
The Tectonics of Venus and Creation
Venus has a nearly perfectly random distribution of craters on its surface. This implies that the Venusian surface is the same age. Astronomers have not found tectonic plates on Venus. How does the
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 72 REFERENCES
Mean age of rifting and volcanism on Venus deduced from impact crater densities
UNLIKE the extensively cratered highlands of the Moon and Mars, the surface of Venus does not preserve a record of heavy bombard-ment from the early history of the Solar System1-3. Those craters that
Aeolian regime of the surface of Venus
Recent probes of the planet Venus reveal a probable surface temperature exceeding 700K and a pressure exceeding 100 atm. A very dusty lower atmosphere may exist which is composed of micron-sized
Magnetism and thermal evolution of the terrestrial planets
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 deg N to 50 deg S, long 60 deg to 310 deg). The
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 the
A New View of the Stratigraphic History of Venus
Abstract Studies of Venus using Magellan data have so far generated two views about the way Venus has evolved. On the one hand, Venus has been suggested to have had a history in which there was a
Venus volcanism: Classification of volcanic features and structures, associations, and global distribution from Magellan data
A preliminary analysis of a global survey of Magellan data covering over 90% of the surface and designed to document the characteristics, location, and dimensions of all major volcanic features on
Mass movements on Venus: Preliminary results from Magellan cycle 1 observations
Mass movements on Venus, seen in radar images acquired by the Magellan spacecraft during its first mapping cycle, are easily interpreted within the scheme commonly used to classify terrestrial
Analysis of regional slope characteristics on Venus and earth.
Regional slope values for earth and Venus are calculated for each 3 o x 3 o region of topography, and the global characteristics of these magnitudes are examined and compared. The effects on
Geologic units on Venus: evidence for their global correlation
...
1
2
3
4
5
...