Hugoniot equations-of-state of oxides representative of deep interiors of extrasolar planets

Details Hugoniot equations-of-state of oxides representative of deep interiors of extrasolar planets Hugoniot equations-of-state of oxides representative of deep interiors of extrasolar planets

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmmr53d..04n&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #MR53D-04

Other

3654 Ultra-High Pressure Metamorphism, 3919 Equations Of State, 3944 Shock Wave Experiments, 5420 Impact Phenomena, Cratering (6022, 8136), 5724 Interiors (8147)

Scientific paper

Shock compression is important for understanding terrestrial and giant planets and their moons, both within and beyond our solar system. Impact-driven shocks enable investigations of microstructural and hydrodynamic/thermodynamic effects similar to those caused by natural impacts on surfaces of such objects. Shock compression of molecular liquids and oxides achieves high pressures and modest temperatures representative of planetary interiors. The pressure and temperature at the bottom of the Earth's mantle are about 130 GPa and 3000 K. This pressure has effectively been an upper limit on pressures to which oxides have been studied experimentally. However, rocky planets larger than Earth have recently been discovered in other solar systems. Oxides in those deep interiors are subjected to pressures and temperatures greater than 130 GPa and 3000 K. Recently, Hugoniot experiments have been performed on the garnet Gd3Ga5O12 (GGG). A phase change is observed at 120 GPa and the high-pressure phase is less compressible than diamond above 170 GPa. Oxides with this structure and composed of more naturally abundant elements might exist and form virtually incompressible cores in large extrasolar rocky planets. Also, GGG will enable higher pressures and lower temperatures in dense metallic fluid hydrogen achieved with shock reverberation than achieved previously with Al2O3 anvils. These states are representative of states deeper in Jovian planets than achieved experimentally thus far with Al2O3 anvils.

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