Erosion of rocky cores in giant gas planets

Details Erosion of rocky cores in giant gas planets Erosion of rocky cores in giant gas planets

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21c1681w&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P21C-1681

Physics

[5724] Planetary Sciences: Fluid Planets / Interiors, [6220] Planetary Sciences: Solar System Objects / Jupiter

Scientific paper

Since giant planets are believed to form by the accumulation of hydrogen-helium gas around a protocore of rock and ice, it is important to understand whether the initial protocore remains stable within the planet or whether it dissolves into the fluid layers of the planet. Building on earlier work which showed the icy portions of the cores of Saturn and Jupiter to be highly soluble within metallic hydrogen at the conditions of these planets' core-mantle boundaries, we now turn our attention to studying the less volatile rocky portions of these cores. Using ab-initio molecular dynamics simulations and coupling constant integration methods, we compute free energies to determine the solubility properties of MgO in fluid hydrogen.

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