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The existence of a proton fluid and an oxygen sub-lattice in the superionic phase raises questions about the response of this phase to electromagnetic stress through protonic fluid motion. Ionic conduction is caused by the movement of negatively or positively charged ions and in the case of high-pressure H 2O ice, protonic conductivity properties are crucial to constrain planetary dynamo processes (e.g., Refs. If dissociation of molecules occurs in water-rich planets, then total conductivity is comprised of an electronic and ionic contribution. Knowing the phases and properties of H 2O at the pressure–temperature ( P–T) conditions of ice giant interiors on their isentropes is critical for validating dynamo simulations-but they are not well understood.Ĭonvection of electrically conducting fluids generates magnetic fields in planetary interiors. Stanley and Bloxham 3, 4 performed numerical dynamo simulations using model geometries to explain Uranus’ and Neptune’s anomalous fields-finding their non-dipolar, non-symmetric magnetic fields are generated by a combination of electromagnetic stresses perturbing the convecting ionic fluid which surrounds a layered, stratified interior. During the visit of the Voyager II spacecraft, its magnetometer revealed surprising non-axisymmetric, non-dipolar magnetic fields for the ice giants that differed substantially from the strong dipolar fields of Jupiter and Saturn 2. During the formation of Uranus and Neptune in the outer region of our solar system, massive amounts of H 2O were accreted and are now stored at hundreds of GPa pressures in their interiors 1. Understanding the phase diagram of H 2O, a ubiquitous molecule in the Universe and a primary building block of volatile-rich giant planets, is of crucial importance for condensed matter physics, solid-state chemistry, and planetary science. This suggests variable and increased electrical conductivity to greater depths in ice giant planets that may promote the generation of multipolar magnetic fields. Although several cubic or orthorhombic structures have been predicted to be the stable structure at these conditions, we show this BCC ice phase is stable to multi-Mbar pressures and temperatures near the melt boundary.
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Here we present X-ray diffraction evidence of a body-centered cubic (BCC) structured H 2O ice at 200 GPa and ~ 5000 K, deemed ice XIX, using the X-ray Free Electron Laser of the Linac Coherent Light Source to probe the structure of the oxygen sub-lattice during dynamic compression. The unusual non-dipolar magnetic fields of ice giant planets, produced by convecting liquid ionic water, are influenced by exotic high-pressure states of H 2O-yet the structure of ice in this state is challenging to determine experimentally.
Saving Earth Britannica Presents Earth’s To-Do List for the 21st Century.Recent discoveries of water-rich Neptune-like exoplanets require a more detailed understanding of the phase diagram of H 2O at pressure–temperature conditions relevant to their planetary interiors.
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