author={Francis Nimmo and Dan McKenzie},
  journal={Annual Review of Earth and Planetary Sciences},
  • F. Nimmo, D. McKenzie
  • Published 1 May 1998
  • Geology, Physics
  • Annual Review of Earth and Planetary Sciences
We review recent developments in the study of volcanism and tectonics on Venus. Venus’s crust is basaltic, dry, and probably about 30 km thick. The mantle convects, giving rise to plumes, and has a similar composition and mean temperature (»1300 ‐ C), but a higher viscosity (»10 20 Pa s), than that of the Earth. Inferred melt generation rates constrain the lithospheric thickness to between 80 and 200 km. The elastic thickness of the lithosphere is about 30 km on average. The present-day lack of… 

Figures from this paper

Rheological decoupling at the Moho and implication to Venusian tectonics
Deformation experiments show that crustal plagioclase is much weaker than mantle olivine at conditions corresponding to the Moho in Venus, and this strength contrast may produce a mechanical decoupling between the Venusian crust and interior mantle convection.
Estimating Venusian thermal conditions using multiring basin morphology
Despite their critical roles in Venus’s geological evolution, neither heat flow through the Venusian lithosphere nor the corresponding tectonic regime in its geological past is well constrained.
Dynamics of fault motion and the origin of contrasting tectonic style between Earth and Venus
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.
Volcanism as an active planetary process on Venus
  • M. Airey
  • Geology, Environmental Science
  • 2015
Volcanism has been a crucial planetary process in the evolution of Venus, shaping the surface and contributing to the formation of the atmosphere and clouds. Some of the key outstanding questions are
Mechanisms for cessation of magmatic resurfacing on Venus
[1] Proposed mechanisms of resurfacing on Venus about 0.3–1 Gyr ago usually involve either some form of tectonic resurfacing in which Venusian lithosphere is recycled mechanically or magmatic
Lithospheric failure on Venus
  • A. Fowler, B. G. O'Brien
  • Geology
    Proceedings of the Royal Society of London. Series A: Mathematical, Physical and Engineering Sciences
  • 2003
We develop a predictive model which has the ability to explain a postulated style of episodic plate tectonics on Venus, through the periodic occurrence of lithospheric subduction events. Present‐day


Constraints on the thermal evolution of Venus inferred from Magellan data
One interpretation of the Magellan data suggests that the cratering record on Venus was erased by a global resurfacing event, or events, the latest ending about 500 m.y. ago. In this
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
Recent deformation rates on Venus
Constraints on the recent geological evolution of Venus may be provided by quantitative estimates of the rates of the principal resurfacing processes, volcanism and tectonism. This paper focuses on
Convection‐driven subsolidus crustal thickening on Venus
We analyze the phenomenon of subsolidus crustal flow in response to mantle convection and test the hypothesis that Venusian crustal plateaus such as Ovda Regio formed over mantle downwellings. We
The gabbro-eclogite phase transition and the elevation of mountain belts on Venus
Maxwell Montes, standing up to 7 km above the adjacent highland plateaus, constitute the highest mountain belt on Venus. Because the thickness of the crust is likely to be limited by the
A tectonic resurfacing model for Venus
Two remarkable aspects of the population of impact craters on Venus are as follows: that craters at all sizes are indistinguishable from a random population; and that the vast majority of craters
The tectonics of Venus
  • W. M. Kaula
  • Geology
    Philosophical Transactions of the Royal Society of London. Series A: Physical and Engineering Sciences
  • 1994
Solid Venus has several differences from solid Earth: a mild variation in topography, with marked departures of some kilometres confined to less than 10% of the surface; no interconnected system of
The tectonic evolution of Western Ishtar Terra, Venus
The origin and evolution of Ishtar Terra is modeled using numerical simulations of crust/mantle interaction on Venus. Based on our modeling, we favor a two phase evolutionary sequence for Ishtar. The