Characterizaton of Materials in Jupiter's Interior with First-Principles Computer Simulations

Details Characterizaton of Materials in Jupiter's Interior with First-Principles Computer Simulations Characterizaton of Materials in Jupiter's Interior with First-Principles Computer Simulations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmmr11a..02m&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #MR11A-02

Physics

5422 Ices, 5430 Interiors (8147), 5724 Interiors (8147)

Scientific paper

Diamond anvil cell experiments have allowed one to make great progress in characterizing planetary ices at high pressure, new phases have been discovered and transformations in chemical bond networks have been identified. However, our understanding is far from complete because conditions near the center of giant planets (<40 Mbar and <20000K for Jupiter) remain beyond the reach of current experimental techniques. A recently developed experimental technique allows one to probe fluids at higher densities than previously attainable. This is achieved by combining static compression in a diamond anvil cell with dynamic laser shock wave experiments. A brief review of theoretically predicted results of such experiments will be given and their importance for planetary interior studies will be discussed. Results from an extensive set of density-functional molecular dynamics simulations will be presented and an equation of state that spans Jupiter's interior is derived. Estimates for the stability of planetary ices will be given. Furthermore interaction effects of dense hydrogen and helium will be analyzed and the validity of commonly assumed linear mixing approximation will be studied. It will be discussed how helium affects the molecular-to- metallic transition in hydrogen and why the presence of helium stabilizes the molecular phase. Furthermore, an updated model for the interior of Jupiter will be described. We discuss our estimates for the heavy element enrichment as well as for the size of Jupiter's core and compare them with previous models based on the Saumon-Chabrier-Van Horn equation of state. 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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