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Title:
Density constraints on the composition of Venus
Authors:
Goettel, K. A.; Shields, J. A.; Decker, D. A.
Affiliation:
AA(Washington University, St. Louis, MO), AB(Washington University, St. Louis, MO), AC(Washington University, St. Louis, MO)
Publication:
In: Lunar and Planetary Science Conference, 12th, Houston, TX, March 16-20, 1981, Proceedings. Section 2. (A82-31677 15-91) New York and Oxford, Pergamon Press, 1982, p. 1507-1516.
Publication Date:
00/1982
Category:
Lunar and Planetary Exploration; Venus
Origin:
STI
NASA/STI Keywords:
Astronomical Models, Density (Mass/Volume), Planetary Composition, Venus (Planet), Chemical Composition, Earth (Planet), Heat Transfer, Iron Oxides, Moments Of Inertia, Planetary Temperature, Planetology, Sulfur
Keywords:
VENUS, EARTH, COMPOSITION, DENSITY
Bibliographic Code:
1982LPSC...12.1507G

Abstract

It is pointed out that the composition of Venus is constrained most directly by the mean density of the planet because the moment of inertia factor is unknown and seismic data do not yet exist for the interior. Values of mass and mean radius give 5.245 g/cu cm for the mean density of Venus. This value is nearly 5% less than the value for the mean density of earth. Explanations for the density difference between Venus and earth are discussed, taking into consideration five models which have been advocated to account for the difference. On the basis of calculations, it is concluded that none of the models can be excluded solely on the basis of the observed density difference between Venus and earth. Therefore, evaluation of the models for Venus must be based principally on the plausibility or implausibility of their constituent assumptions and on the success of the models in predicting the compositions of other planets for which more data exist.

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