Behavior of Ammonia and Water at High Pressure and Temperature, Implications in Planetary Physics.

Details Behavior of Ammonia and Water at High Pressure and Temperature, Implications in Planetary Physics. Behavior of Ammonia and Water at High Pressure and Temperature, Implications in Planetary Physics.

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..mar.i3409c&link_type=abstract

American Physical Society, Annual March Meeting, March 16-20, 1998 Los Angeles, CA, abstract #I34.09

Physics

Scientific paper

Planetary probes are bringing fresh information on the atmospheric composition of the outer planets of the solar system. However, most of the phenomena relevant for the physics of these planets (such as their composition, or the origin of their magnetic field) take place at ultra high pressure and temperature beneath the surface and are not directly accessed by these probes. We have recently shown that computer simulations ( Ancilotto et al. Science 275 1288, 1997 ) can be extremely helpful for understanding some fundamental aspects of the physics of planetary interiors. Using variable-cell first principles molecular dynamics we have investigated the behavior of NH3 and H_2O at pressure and temperature typical of the middle ``ice'' layers of Uranus and Neptune, from ~ 20 GPa -- 2000 K in the outer part, to 300 GPa -- 5000 K near the rocky core ( Hubbard, Science 275 1279, 1997 ) . In our simulations we find new super-ionic and metallic phases both for NH3 and H_2O, supporting the hypothesis that the magnetic field for those planets is originated in the middle ice layer. Computed values for the conductivity agree with those obtained in shock-wave experiments ( Nellis, Science 240 779, 1988).

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