Anderson, Don L. (1980) Tectonics and composition of Venus. Geophysical Research Letters, 7 (1). pp. 101-102. ISSN 0094-8276. doi:10.1029/GL007i001p00101. https://resolver.caltech.edu/CaltechAUTHORS:20150220-143637545
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Abstract
The uncompressed density of Venus is a few percent less than the Earth. The high upper mantle temperature of Venus deepens the eclogite stability field and inserts a partial melt field. A thick basaltic crust is therefore likely. The anomalous density of Venus relative to the progression from Mercury to Mars may therefore have a tectonic rather than a cosmo-chemical explanation. There may be no need to invoke differences in composition or oxidization state.
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Additional Information: | © 1980 by the American Geophysical Union. Paper number 9L1659. Received September 17, 1979; accepted November 27, 1979. I would like to thank J. V. Smith, W. Kaula and E. Stolper for helpful comments on the original manuscript. This research was supported by NASA Contract No. NGL-05-002-069. Contribution No. 3291, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125. | |||||||||
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Issue or Number: | 1 | |||||||||
DOI: | 10.1029/GL007i001p00101 | |||||||||
Record Number: | CaltechAUTHORS:20150220-143637545 | |||||||||
Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20150220-143637545 | |||||||||
Official Citation: | (1980), Tectonics and composition of Venus. Geophysical Research Letters, 7: 101–102. doi: 10.1029/GL007i001p00101 | |||||||||
Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | |||||||||
ID Code: | 55071 | |||||||||
Collection: | CaltechAUTHORS | |||||||||
Deposited By: | Tony Diaz | |||||||||
Deposited On: | 23 Feb 2015 20:03 | |||||||||
Last Modified: | 10 Nov 2021 20:41 |
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