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Published 1976 | public
Book Section - Chapter

Interior models of Jupiter

Abstract

Understanding the interior of Jupiter depends upon our knowledge of the thermodynamics and transport properties of hydrogen-helium mixtures at high pressures and temperatures. The current status of this knowledge is reviewed, and attention is given to the metallic-molecular hydrogen transition and the limited solubility of helium in hydrogen. Models of Jupiter are constructed which are consistent with all the observations to date, but which make various assumptions about the thermodynamics and composition of the interior. These models typically consist of a rocky core surrounded by a nearly-solar fluid mixture. In contrast to the models of Podolak and Cameron, a large enhancement of water or helium is not found to be essential. It is concluded that further progress in constructing interior models requires a better understanding of the thermodynamics of dense molecular hydrogen.

Additional Information

© 1976 University of Arizona Press. Discussions with A. G. W. Cameron, W. C. DeMarcus, and W. B. Hubbard are gratefully acknowledged. This work is supported by the NSF Grants MPS72-05056-A02, MPS74-17838 and NASA Grant NGR-33-010-188.

Additional details

Created:
August 22, 2023
Modified:
October 24, 2023