LASP Research Shows Saturn’s Moon May Harbor Hydrothermal Activity

Measurements from NASA’s Cassini spacecraft suggest that Saturn’s moon Enceladus, which has jets of water vapor and ice gushing from its south pole, also harbors a large interior ocean with hydrothermal activity beneath an ice shell, as this illustration depicts. Image Credit: NASA/JPL-Caltech

Measurements from NASA’s Cassini spacecraft suggest that Saturn’s moon Enceladus, which has jets of water vapor and ice gushing from its south pole, also harbors a large interior ocean with hydrothermal activity beneath an ice shell, as this illustration depicts. Image Credit: NASA/JPL-Caltech

March 13, 2015 – Scientists with NASA’s Cassini mission, led by LASP and University of Colorado postdoctoral researcher, Sean Hsu, have found that microscopic grains of rock detected near Saturn imply hydrothermal activity is taking place within the planet’s moon Enceladus. The results were published this week in the journal Nature.

This is the first clear indication of an icy moon having hydrothermal activity—in which seawater infiltrates and reacts with a rocky crust, emerging as a heated, mineral-laden solution. The implications of such activity on a world other than our planet open up unprecedented scientific possibilities.

“These findings add to the possibility that Enceladus, which contains a subsurface ocean and displays remarkable geologic activity, could contain environments suitable for living organisms,” said John Grunsfeld, astronaut and associate administrator of NASA’s Science Mission Directorate in Washington. “The locations in our solar system where extreme environments occur in which life might exist may bring us closer to answering the question: are we alone in the universe.”

An extensive, four-year analysis of data from the spacecraft, computer simulations and laboratory experiments led researchers to the conclusion the tiny grains most likely form when hot water containing dissolved minerals from the moon’s rocky interior travels upward, coming into contact with cooler water. Temperatures required for the interactions that produce the tiny rock grains would be at least 194 degrees Fahrenheit (90 degrees Celsius).

“It’s very exciting that we can use these tiny grains of rock, spewed into space by geysers, to tell us about conditions on—and beneath—the ocean floor of an icy moon,” said Hsu, who served as lead author on the paper.

Cassini’s cosmic dust analyzer (CDA) instrument repeatedly detected minuscule rock particles, rich in the element silicon, orbiting Saturn at the same distance as Enceladus. By process of elimination, the CDA team concluded these particles must be grains of silica, which is found on Earth in sand and the mineral quartz. The consistent size of the grains observed by Cassini—the largest of which were 6 to 9 nanometers—was the clue that told the researchers a specific process likely was responsible.

On Earth, the most common way to form silica grains of this size is hydrothermal activity involving a specific range of conditions; namely, when slightly alkaline water with modest salinity that is super-saturated with silica undergoes a big drop in temperature.

“We methodically searched for alternate explanations for the nanosilica grains, but every new result pointed to a single, most likely origin,” said Frank Postberg, a Cassini CDA team scientist at Heidelberg University in Germany, and a co-author on the paper.

Hsu and Postberg worked closely with colleagues at the University of Tokyo, who performed the detailed laboratory experiments that validated the hydrothermal activity hypothesis. The Japanese team, led by Yasuhito Sekine, verified the conditions under which silica grains form at the same size Cassini detected. The researchers think these conditions may exist at the seafloor on Enceladus, where hot water from the interior meets the relatively cold water at the ocean bottom.

The extremely small size of the silica particles also suggests that they travel upward relatively quickly from their hydrothermal origin to the near-surface sources of the moon’s now famous geysers. From seafloor to outer space, a distance of about 30 miles (50 kilometers), the grains spend a few months to a few years in transit, otherwise they would grow to much larger sizes.

Cassini first revealed active geology on Enceladus in 2005 with evidence of an icy spray issuing from the moon’s south polar region and higher than expected temperatures in the icy surface there. The mission soon revealed a towering plume of water ice and vapor, salts and organic materials that issues from relatively warm fractures on the wrinkled surface. Gravity science results published in 2014 strongly suggest the presence of a 6-mile- (10-kilometer-) deep ocean beneath an ice shell about 19 to 25 miles (30 to 40 kilometers) thick.

The authors point out that Cassini’s gravity measurements suggest Enceladus’ rocky core is quite porous, which would allow water from the ocean to percolate into the interior. This would provide a huge surface area where rock and water could interact.

“It’s possible much of this interesting hot-water chemistry occurs deep inside the moon’s core,” Hsu said.

Co-authors of the Nature paper include CU-Boulder Professor Mihaly Horanyi and Assistant Professor Sascha Kempf of the Laboratory for Atmospheric and Space Physics (LASP) of Boulder, Colorado. Both also are faculty members in CU-Boulder’s physics department and co-investigators of the Cassini CDA. The online version of the publication can be found here: http://dx.doi.org/10.1038/nature14262.

In another paper, published in Geophysical Research Letters last month, Cassini scientists also reported on the abundance of methane spewing into the atmosphere of Enceladus. The finding is the result of extensive modeling by French and American scientists to address why methane, as previously sampled by Cassini, is curiously abundant in the plume.

This illustration depicts potential origins of methane found in the plume of gas and ice particles that sprays from Saturn's moon, Enceladus, based on research by scientists working with the Ion and Neutral Mass Spectrometer on NASA's Cassini mission. Image Credit: Southwest Research Institute

This illustration depicts potential origins of methane found in the plume of gas and ice particles that sprays from Saturn’s moon, Enceladus, based on research by scientists working with the Ion and Neutral Mass Spectrometer on NASA’s Cassini mission. Image Credit: Southwest Research Institute

The team found that, at the high pressures expected in the moon’s ocean, icy materials called clathrates could form that imprison methane molecules within a crystal structure of water ice. Their models indicate that this process is so efficient at depleting the ocean of methane that the researchers still needed an explanation for its abundance in the plume.

In one scenario, hydrothermal processes super-saturate the ocean with methane. This could occur if methane is produced faster than it is converted into clathrates. A second possibility is that methane clathrates from the ocean are dragged along into the erupting plumes and release their methane as they rise, like bubbles forming in a popped bottle of champagne.

The authors agree both scenarios are likely occurring to some degree, but they note that the presence of nanosilica grains, as documented by the other paper, favors the hydrothermal scenario.

“We didn’t expect that our study of clathrates in the Enceladus ocean would lead us to the idea that methane is actively being produced by hydrothermal processes,” said lead author Alexis Bouquet, a graduate student at the University of Texas at San Antonio. Bouquet worked with co-author Hunter Waite, who leads the Cassini Ion and Neutral Mass Spectrometer (INMS) team at Southwest Research Institute in San Antonio.

The Cassini-Huygens mission is a cooperative project of NASA, ESA (European Space Agency) and the Italian Space Agency. NASA’s Jet Propulsion Laboratory in Pasadena, California, manages the mission for the agency’s Science Mission Directorate in Washington. The Cassini CDA instrument was provided by the German Aerospace Center. The instrument team, led by Ralf Srama, is based at the University of Stuttgart in Germany. JPL is a division of the California Institute of Technology in Pasadena.