Thermodynamics of dense hydrogen-helium fluids

Details Thermodynamics of dense hydrogen-helium fluids Thermodynamics of dense hydrogen-helium fluids

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..255g&link_type=abstract

Astrophysical Journal, vol. 199, July 1, 1975, pt. 1, p. 255-264. AEC-sponsored research

Physics

10

Astronomical Models, Helium, Hydrogen, Planetary Composition, Stellar Structure, Thermodynamic Properties, Abundance, Density Distribution, Gas Density, Gas Mixtures, Planetary Temperature, Solar Physics, Stellar Mass, Thomas-Fermi Model

Scientific paper

The equilibrium thermodynamic properties of hydrogen-helium fluids are studied in the density-temperature regime appropriate to the interiors of evolving very low-mass stars and giant planets. The low-density molecular fluid is treated by a free energy minimization method utilizing several theoretical models and recent high-pressure experimental results for hydrogen. The high-density metallic fluid is treated by an extension of Thomas-Fermi theory. These approaches are combined to yield a detailed thermodynamic description for two fluids: pure hydrogen and a solar mixture. Equations of state are given for the density range from 0.0001 to 0.001 gm/cu cm and a temperature range from 200 to 60,000 K.

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