Researchers mimic high-pressure form of ice found in giant icy moons

Article written: 4 Mar , 2006
Updated: 24 Mar , 2012

Jupiter’s icy moon Callisto. Image credit: NASA Click to enlarge
As scientists learn more about our Solar System, they’ve found water ice in some unusual situations. One of the most intriguing of these environments is on icy moons, like Jupiter’s Europa, and Uranus’ Triton. Researchers at the Lawrence Livermore National Laboratory have recreated this kind of ice in their laboratory; ice that probably mimics the conditions of pressure, temperature, stress, and grain size found on these moons. This ice can slowly creep and swirl around depending on the temperature of the moons’ interiors.

That everyday ice you use to chill your glass of lemonade has helped researchers better understand the internal structure of icy moons in the far reaches of the solar system.

A research team has demonstrated a new kind of “creep,” or flow, in a high-pressure form of ice by creating in a laboratory the conditions of pressure, temperature, stress, and grain size that mimic those in the deep interiors of large icy moons.

High-pressure phases of ice are major components of the giant icy moons of the outer solar system: Jupiter’s Ganymede and Callisto, Saturn’s Titan, and Neptune’s Triton. Triton is roughly the size of our own moon; the other three giants are about 1.5 times larger in diameter. Accepted theory says that most of the icy moons condensed as “dirty snowballs” from the dust cloud around the sun (the solar nebula) about 4.5 billion years ago. The moons were warmed internally by this accretionary process and by radioactive decay of their rocky fraction.

The convective flow of ice (much like the swirls in a hot cup of coffee) in the interiors of the icy moons controlled their subsequent evolution and present-day structure. The weaker the ice, the more efficient the convection, and the cooler the interiors. Conversely, the stronger the ice, the warmer the interiors and the greater the possibility of something like a liquid internal ocean appearing.

The new research reveals in one of the high-pressure phases of ice (“ice II”) a creep mechanism that is affected by the crystallite or “grain” size of the ice. This finding implies a significantly weaker ice layer in the moons than previously thought. Ice II first appears at pressures of about 2,000 atmospheres, which corresponds to a depth of about 70 km in the largest of the icy giants. The ice II layer is roughly 100 km thick. The pressure levels at the centers of the icy giant moons eventually reach the equivalent of 20,000 to 40,000 Earth atmospheres.

Researchers from Lawrence Livermore National Laboratory (LLNL), Kyushu University in Japan and the U.S. Geological Survey conducted creep experiments using a low-temperature testing apparatus in the Experimental Geophysics Laboratory at LLNL. They then observed and measured ice II grain size using a cryogenic scanning electron microscope. The group found a creep mechanism that dominates flow at lower stresses and finer grain sizes. Earlier experiments at higher stresses and larger grain size activated flow mechanisms that did not depend on grain size.

The experimentalists were able to prove that the new creep mechanism was indeed related to the size of the ice grains, something that previously had only been examined theoretically.

But the measurement was no easy feat. First, they had to create ice II of very fine grain size (less than 10 micrometers, or one-tenth the thickness of a human hair). A technique of rapid cycling of pressure above and below 2,000 atmospheres eventually did the trick. Adding to that, the team maintained a very steady 2,000 atmospheres of pressure within the testing apparatus to run a low-stress deformation experiment for weeks on end. Finally, to delineate the ice II grains and make them visible in the scanning electron microscope, the team developed a method of marking the grain boundaries with the common form of ice (“ice I”), which appeared different from ice II in the microscope. Once the boundaries were identified, the team could measure ice II’s grain size.

“These new results show that the viscosity of a deep icy mantle is much lower than we previously thought,” said William Durham, a geophysicist in Livermore’s Energy and Environment Directorate.

Durham said the high-quality behavior of the test apparatus at 2,000 atmospheres pressure, the collaboration with Tomoaki Kubo of Kyushu University, and success in overcoming serious technical challenges made for a fortuitous experiment.

Using the new results, the researchers conclude that it is likely the ice deforms by the grain size-sensitive creep mechanism in the interior of icy moons when the grains are up to a centimeter in size.

“This newly discovered creep mechanism will change our thinking of the thermal evolution and internal dynamics of medium- and large-size moons of the outer planets in our solar system,” Durham said. “The thermal evolution of these moons can help us explain what was happening in the early solar system.”

The research appears in the March 3 issue of the journal Science.

Founded in 1952, Lawrence Livermore National Laboratory has a mission to ensure national security and apply science and technology to the important issues of our time. Lawrence Livermore National Laboratory is managed by the University of California for the U.S. Department of Energy’s National Nuclear Security Administration.

Original Source: LLNL News Release

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