The structure and evolution of Jupiter - The fluid contraction stage

Details The structure and evolution of Jupiter - The fluid contraction stage The structure and evolution of Jupiter - The fluid contraction stage

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..265g&link_type=abstract

Astrophysical Journal, vol. 199, July 1, 1975, pt. 1, p. 265-281. AEC-NASA-sponsored research

Physics

Fluid Dynamics

46

Astronomical Models, Fluid Dynamics, Jupiter (Planet), Planetary Evolution, Planetary Structure, Thermodynamic Properties, Atmospheric Models, Contraction, Planetary Mass, Stellar Evolution, Stellar Mass, Stellar Structure

Scientific paper

The complete evolution of a contracting star of Jovian mass consisting of a convective adiabatic homogeneous fluid is determined using stellar structure methods, improved model atmosphere calculations, and substantially improved thermodynamic properties for hydrogen and hydrogen-helium fluids. The model atmospheres are calculated in the form of time-averaged vertical temperature structures, including all relevant sources of opacity and a solar energy deposition component, and the thermodynamic properties are modified to obtain better agreement with Monte Carlo results for metallic fluids. The resultant gravitationally contracting evolutionary models are found to have two phases: an early stellar phase similar to a typical low-mass pre-main-sequence body and a later phase constituting an approach to a degenerate-dwarf cooling curve. The first phase is shown to have high luminosities and internal temperatures, while the second gives excellent agreement with the observed radius and luminosity of Jupiter. Analysis indicates that the equation of state and superadiabaticity have the strongest influence on evolution over planetary time scales.

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