Modeling Jupiter's Interior with a Hydrogen-Helium Equation of State Derived From First Principles Computer Simulations

Details Modeling Jupiter's Interior with a Hydrogen-Helium Equation of State Derived From First Principles Computer Simulations Modeling Jupiter's Interior with a Hydrogen-Helium Equation of State Derived From First Principles Computer Simulations

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p52a..03m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P52A-03

Physics

5724 Interiors (8147), 5749 Origin And Evolution, 6220 Jupiter, 8147 Planetary Interiors (5430, 5724, 6024)

Scientific paper

We report results from recent investigations of the interior structure of Jupiter 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 the 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 presence 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. 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. 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. 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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