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Tectonics and composition of Venus

Anderson, Don L. (1980) Tectonics and composition of Venus. Geophysical Research Letters, 7 (1). pp. 101-102. ISSN 0094-8276. doi:10.1029/GL007i001p00101.

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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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Caltech Division of Geological and Planetary Sciences3291
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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
Deposited By: Tony Diaz
Deposited On:23 Feb 2015 20:03
Last Modified:10 Nov 2021 20:41

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