J. Phys. IV France
Volume 139, December 2006
Page(s) 9 - 19
From Regional Climate Modelling to the Exploration of Venus
C. Boutron
J. Phys. IV France 139 (2006) 9-19

DOI: 10.1051/jp4:2006139003

Venus: Divergent outcomes of terrestrial planet formation

E.R. Stofan

Proxemy Research, Rectortown VA 20140, USA & Department of Earth Sciences, UCL, Gower St., London WC1E 6BT, UK

(Published online: 9 January 2007)

Although Venus is often referred to as the most Earth-like of the terrestrial planets, its runaway greenhouse has resulted in a dry, hot, uninhabitable surface. Its surface geology is complex, with volcanoes ranging from <5 to >500 km across, lava flows fields >800 km across, mountain belts, rift zones, and terrains unique to Venus such as tesserae and coronae. It surface has an average crater retention age similar to Earth's continents, but the random nature of the impact crater population renders it useless in providing time constraints for the geologic history of Venus. At some point in the past, Venus lost an ocean's worth of water. If this water persisted on the surface for long periods of time in Venus's early history, life may have evolved. Untangling the complex history of Venus, and what it reveals for the evolution of habitable planets, will require future missions to the surface.

© EDP Sciences 2006