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The phase diagram and transport properties for hydrogen-helium fluid planets

Stevenson, D. J. and Salpeter, E. E. (1977) The phase diagram and transport properties for hydrogen-helium fluid planets. Astrophysical Journal Supplement Series, 35 (10). pp. 221-237. ISSN 0067-0049. http://resolver.caltech.edu/CaltechAUTHORS:20131118-133823616

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Abstract

Hydrogen and helium are the major constituents of Jupiter and Saturn, and phase transitions can have important effects on the planetary structure. In this paper, the relevant phase diagrams and microscopic transport properties are analyzed in detail. The following paper (Paper II) applies these results to the evolution and present dynamic structure of the Jovian planets. Pure hydrogen is first discussed, especially the nature of the molecular-metallic transition and the melting curves for the two phases. It is concluded that at the temperatures and pressures of interest (T ≈ 10^4 K, P ≈ 1-10 Mbar), both phases are fluid, but the transition between them might nevertheless be first-order. The insulator-metal transition in helium occurs at a much higher pressure (~ 70 Mbars) and is not of interest. The phase diagrams for both molecular and metallic hydrogen-helium mixtures are discussed. In the metallic mixture, calculations indicate a miscibility gap for T ≾ 10^4 K. Immiscibility in the molecular mixture is more difficult to predict but almost certainly occurs at much lower temperatures. A fluid-state model is constructed which predicts the likely topology of the threedimensional phase diagram. The greater solubility of helium in the molecular phase leads to the prediction that the He/H mass ratio is typically twice as large in the molecular phase as in the coexisting metallic phase. Under these circumstances a "density inversion" is possible in which the molecular phase becomes more dense than the metallic phase. The partitioning of minor constituents is also considered: The deuterium/hydrogen mass ratio is essentially the same for all coexisting hydrogen-helium phases, at least for T ≳ 5000 K. The partitioning of H_2O, CH_4, and NH_3 probably favors the molecular (or helium-rich) phase. Substances with high conduction electron density (e.g., AI) may partition into the metallic phase. Electronic and thermal conductivities, viscosity, helium diffusivity, and Soret coefficient are evaluated for the fluid molecular and metallic phases, all to at least order-of-magnitude accuracy. The properties of the metallic phase are typical of a liquid alkali metal, and those of the molecular phase are typical of a dense neutral fluid (except that the conductivities may be almost metallic at the transition pressure). The opacities of molecular hydrogen and solar-composition mixtures are discussed for T ≈ 500 K, where molecular hydrogen alone may be insufficiently opaque to ensure convection in the Jovian planets. Sufficient opacity to initiate convection is probably supplied by the minor constituents. Current uncertainties are assessed.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://adsabs.harvard.edu/abs/1977ApJS...35..221SADSArticle
http://dx.doi.org/10.1086/190478DOIArticle
ORCID:
AuthorORCID
Stevenson, D. J.0000-0001-9432-7159
Additional Information:© 1977 American Astronomical Society. Received 1976 June 23; accepted 1977 April 13. We wish to thank N. W. Ashcroft, M. E. Fisher, W. B. Hubbard, and R. Smoluchowski for discussions and comments. This work is supported by National Aeronautics and Space Administration grant NGR 33-010-188 and National Science Foundation grant AST 75-21153.
Funders:
Funding AgencyGrant Number
NASANGR 33-010-188
NSFAST 75-21153
Subject Keywords:equation of state; planets: interiors
Record Number:CaltechAUTHORS:20131118-133823616
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20131118-133823616
Official Citation:The phase diagram and transport properties for hydrogen-helium fluid planets Stevenson, D. J.; Salpeter, E. E. Astrophysical Journal Supplement Series, vol. 35, Oct. 1977, p. 221-237.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42530
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:18 Nov 2013 22:05
Last Modified:13 Feb 2019 18:05

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