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E.R. Stofan (Jet Propulsion Laboratory, California Institute of Technology), J.E. Guest (University College London)
Two views about the way Venus has evolved have been generated from studies of Magellan data. Venus has been suggested to have had a history in which there was a series of epochs each represented by a different volcanic or tectonic process on a global scale (e.g., Basilevsky et al. 1997). However, there is evidence to suggest that coronae, rifts, wrinkle ridges, small and large edifices, and large flow fields have each formed throughout the portion of Venus' history revealed by presently exposed rock units (Guest and Stofan, 1999). We propose that the plains have been built up by lavas erupted in a number of different styles, each occurring throughout the history represented by the exposed stratigraphy of the planet. The low number and apparent randomness of the impact crater population has left us with an inability to date individual terrains on Venus. Dates derived from crater counts accumulated from the combined area of specific types of feature such as coronae (e.g., Price et al. 1996), must be interpreted with care as the method is based upon the assumption that features of like morphology have the same age. Additional problems arise with features such as corona and large volcanoes, where late-stage volcanic flows mask evidence of the timing of the initiation of the feature with respect to surrounding units. Our detailed studies indicate that Venus has had a complex history in which most geologic processes have operated in a non-directional fashion to a greater or lesser extent throughout the planet's history.