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The Influence of the Surface Boundary Layer on Evolutionary Models of Jupiter∗

Published online by Cambridge University Press:  14 August 2015

Harold C. Graboske Jr.
Harold C. Graboske Jr.*
Affiliation:
Lawrence Livermore Laboratory, Livermore, Calif., U.S.A.

Abstract

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A recent theoretical study of the structure and evolution of Jupiter (Graboske et al., 1974b) is based on a three-stage model of Jovian evolution. The central phase, gravitational contraction of an adiabatic, homogeneous convective fluid system, begins early in solar system evolution and lasts for times of the order of 2 × 109 yr. Good agreement with observed radius and luminosity is achieved for a model with a solar mixture composition. The surface boundary layer has a dominant influence on the evolutionary timescale. Surface boundary factors which are important are the solar energy input, a function of the solar luminosity and the planetary albedo, and the detailed physics of the superadiabatic zone, which depends on the variation of opacity and ∇ad with depth. The evolutionary study demonstrates that the current planet cannot be an adiabatic homogeneous fluid throughout. The inclusion of a superadiabatic zone is necessary, and the existence of a heterogeneous (gravitationally layered) fluid interior is possible.

Type
Part III Outer Planets and Their Satellites
Information
Symposium - International Astronomical Union , Volume 65: Exploration of the Planetary System , 1974 , pp. 337 - 344
Copyright
Copyright © Reidel 1974 

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