Melting behavior of H<sub>2</sub>O at high pressures and temperatures

Jung‐Fu Lin, Eugene Gregoryanz, Viktor V. Struzhkin, Maddury Somayazulu, Ho‐kwang Mao, Russell J. Hemley

doi:10.1029/2005gl022499

Melting behavior of H<sub>2</sub>O at high pressures and temperatures

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Jung‐Fu Lin

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA
Eugene Gregoryanz

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA
Viktor V. Struzhkin

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA
Maddury Somayazulu

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA
Ho‐kwang Mao

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA
Russell J. Hemley

Geophysical Laboratory Carnegie Institution of Washington Washington, D. C. USA

書誌事項

公開日: 2005-06

権利情報

http://onlinelibrary.wiley.com/termsAndConditions#vor

DOI

10.1029/2005gl022499

公開者: American Geophysical Union (AGU)

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説明

<jats:p>Water plays an important role in the physics and chemistry of planetary interiors. In situ high pressure‐temperature Raman spectroscopy and synchrotron x‐ray diffraction have been used to examine the phase diagram of H<jats:sub>2</jats:sub>O. A discontinuous change in the melting curve of H<jats:sub>2</jats:sub>O is observed at approximately 35 GPa and 1040 K, indicating a triple point on the melting line. The melting curve of H<jats:sub>2</jats:sub>O increases significantly above the triple point and may intersect the isentropes of Neptune and Uranus. Solid ice could therefore form in stratified layers at depth within these icy planets. The extrapolated melting curve may also intersect with the geotherm of Earth's lower mantle above 60 GPa. The presence of solid H<jats:sub>2</jats:sub>O would result in a jump in the viscosity of the mid‐lower mantle and provides an additional explanation for the observed higher viscosity of the mid‐lower mantle.</jats:p>