Properties of planetary fluids at high pressures and temperatures

Details Properties of planetary fluids at high pressures and temperatures Properties of planetary fluids at high pressures and temperatures

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept...29n&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 29-31 (SEE N92-10728 01-91)

Physics

Geophysics

Chemical Composition, Density Distribution, High Pressure, High Temperature, Planetary Composition, Planetary Cores, Planetary Magnetic Fields, Ammonia, Electrical Resistivity, Equations Of State, Gas Giant Planets, Helium, Hydrogen, Ice, Methane, Water

Scientific paper

Observational data obtained by the Voyager space probes to the giant planets Jupiter, Saturn, Uranus, and Neptune have provided valuable information, which is used to refine the picture of the nature of the interiors of these planets. Major results from the Voyager missions include observations of substantial magnetic fields and improved models of internal density distributions. The goal is to obtain equations of state and electrical conductivity data for planetary gases (H2 and He) and the ices (H2O, CH4, and NH3, and their mixtures), which are considered to be the major constituents of the giant planets. These data are needed to test theoretical data bases used to construct models of the chemical composition of planetary interiors, models which are consistent with observables such as mass, diameter, gravitational moments, rotation rate, and magnetic field. The 100 GPa (1 Mbar) pressures and several 1000 K temperatures in the giant planets can be achieved in the lab by the shock compression of liquid specimens. Results are briefly examined.

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