Solubility of Water Ice in Metallic Hydrogen: Consequences for Core Erosion in Gas Giant Planets

Details Solubility of Water Ice in Metallic Hydrogen: Consequences for Core Erosion in Gas Giant Planets Solubility of Water Ice in Metallic Hydrogen: Consequences for Core Erosion in Gas Giant Planets

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...745...54w&link_type=abstract

The Astrophysical Journal, Volume 745, Issue 1, article id. 54 (2012).

Astronomy and Astrophysics

Astronomy

3

Planets And Satellites: Dynamical Evolution And Stability, Planets And Satellites: Individual: Jupiter Saturn, Planets And Satellites: Interiors

Scientific paper

Using ab initio simulations we investigate whether water ice is stable in the cores of giant planets, or whether it dissolves into the layer of metallic hydrogen above. By Gibbs free energy calculations we find that for pressures between 10 and 40 Mbar the ice-hydrogen interface is thermodynamically unstable at temperatures above approximately 3000 K, far below the temperature of the core-mantle boundaries in Jupiter and Saturn. This implies that the dissolution of core material into the fluid layers of giant planets is thermodynamically favored, and that further modeling of the extent of core erosion is warranted.

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