Mathematics – Logic
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..239o&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Mathematics
Logic
Scientific paper
ABSTRACT Two main groups of models have been proposed to explain the statistical distribution of craters on Venus [1, 2]. Schaber et al. [1] proposed that » 500 million years ago (the mean surface age of the planet, T) Venus underwent catastrophic resurfacing followed by relatively minor resurfacing rates since then. The stratigraphic analysis by Basilevsky and Head [3] is generally consistent with this model. They argue that the duration of resurfacing was relatively short, » 0:1T. Phillips et al. [2] presented an alternative model according to which the equilibrium population of craters is a result of small-scale resurfacing that occurred in different places of the planet at different times. According to the statistical analysis of crater distribution by Hauck et al. [4] the duration of resurfacing may be up to » 0:5T Various geodynamical models have been proposed to explain the mechanisms of resurfacing [5-13]. Reese et al. [13] argued that the models of magmatic resurfacing have the strongest observational and theoretical support. They showed that in the absence of plate tectonics, Venus was likely to be substantially melted by radiogenic heating during some of its history and that the resurfacing "event" may simply reflect the waning stages of the cessation of magmatism. To test this hypothesis further we focus on the very last stages of magmatism (the observable history of Venus), that is from the time when "dry" patches began to appear. Here we consider a spherical model of cooling history of Venus starting with the first appearance of dry patches and calculate the evolution of volcanism using different sets of assumptions, regarding the intensity of convection, initial temperature, and initial lid thickness. The goal is to determine the evolution of volcanic activity on Venus and compare the results to geologic observations.
Head James W.
Orth C. P.
Reese C. C.
Solomatov Viatcheslav S.
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