Jupiter and Saturn Interior Models with an Equation of State Derived From First Principles Computer Simulations

Details Jupiter and Saturn Interior Models with an Equation of State Derived From First Principles Computer Simulations Jupiter and Saturn Interior Models with an Equation of State Derived From First Principles Computer Simulations

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.0204h&link_type=abstract

American Astronomical Society, DPS meeting #38, #02.04; Bulletin of the American Astronomical Society, Vol. 38, p.483

Astronomy and Astrophysics

Astronomy

Scientific paper

We report results from recent investigations of the interior structures of Jupiter and Saturn using state-of-the-art computer simulations of dense fluid hydrogen and helium. Thermodynamic properties used in the models were obtained using density-functional molecular dynamics (DFT-MD) simulations on a grid of temperature and density points spanning the interiors of these planets.
In addition to calculations for pure hydrogen, simulation results for the different concentrations of hydrogen-helium mixtures are presented. The corrections to the commonly used linear mixing approximation are characterized, and it is demonstrated how the addition of helium increases the stability of the molecular phase of hydrogen.
Our interior models update the suite of models that were based on the widely used Saumon-Chabrier-Van Horn (SCVH) equation of state for hydrogen and helium. Unlike SCVH, the computed DFT-EOS does not predict any first-order thermodynamic discontinuities associated with pressure-dissociation and metallization of hydrogen. Instead, the DFT-EOS predicts that the molecular dissociation leads intermediate decrease in pressure, which has profound effects on the thermodynamic properties in a zone approximately 6000 km below the 1-bar level in Jupiter and 1100 km below that level in Saturn.
Deviations of the DFT-EOS from SCVH are up to about +/- 5% depending on the pressure, and thus affect interior models at the same level as possible effects of a jovian core. We will discuss inferred core masses and interior metallicity for Jupiter and Saturn. Our results will eventually aid in interpretation of data expected from the Juno orbiter mission.
Supported by NASA PGG Grants NAG5-13775 and PGG04-0000-0116 and NSF Grant 0507321.

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