Characterization of Jupiter's Interior with First Principles Computer Simulations

Details Characterization of Jupiter's Interior with First Principles Computer Simulations Characterization of Jupiter's Interior with First Principles Computer Simulations

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aps..mara23001m&link_type=abstract

American Physical Society, APS March Meeting, March 5-9, 2007, abstract #A23.001

Physics

Scientific paper

We report results from recent investigations of the interior structures of Jupiter using density-functional molecular dynamics (DFT) simulations of dense fluid hydrogen-helium mixtures [1]. The equation of state (EOS) is derived on a grid of temperature and density points spanning Jupiter's interiors. The properties of both fluids in dynamic shock compression experiments are compared [2]. Based on the DFT-EOS, we derive models for the interior of giant planets. Our models update the suite of models that were based on the widely used Saumon-Chabrier-Van Horn (SCVH) EOS. Unlike SCVH, the computed DFT-EOS does not predict any first-order thermodynamic discontinuities associated with pressure-dissociation and metallization of hydrogen. Deviations of the DFT-EOS from SCVH are up to about +/- 5% depending on the pressure. As a result our models predict a significantly larger rocky core for Jupiter than SCVH. We will discuss inferred core mass and make predictions for properties of core. [1] J. Vorberger, I. Tamblyn, B. Militzer, S.A. Bonev, ``Hydrogen-Helium Mixtures in the Interiors of Giant Planets,'' cond-mat/0609476. [2] B. Militzer, PRL 97 (2006) 175501. Supported by NASA PGG04-0000-0116 and NSF Grant 0507321.

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