Icy Tendrils in Saturn’s E Ring Traced Back to Enceladus

Cassini images of Enceladus in the E ring (top left, upper center) and computer-generated models of the same scenes. Views from 2006 and 2013, respectively. (NASA/JPL-Caltech/Space Science Institute)

Cassini images of Enceladus in the E ring (top left, upper center) and computer-generated models of the same scenes. Views from 2006 and 2013, respectively. (NASA/JPL-Caltech/Space Science Institute)

As the ice-encrusted moon Enceladus makes it way along its orbit around Saturn it gets repeatedly squeezed by the giant planet’s gravity, like a frozen stress ball with water-filled insides. This constant squeezing and relaxing generates friction heat in the moon’s crust, which could be responsible for keeping some of its internal water liquid and spraying it out into space from long canyons that cut across its southern pole. And sometimes more ice gets shot out than at other times, forming a trail of long tendrils that stretch into the “E” ring – a hazy, diffuse doughnut around Saturn made from Enceladus’ icy exhaust.

These tendrils had been observed by the Cassini spacecraft since 2006, but only now have they been positively confirmed to be the results of specific geysers on the 318-mile-wide moon.

“We’ve been able to show that each unique tendril structure can be reproduced by particular sets of geysers on the moon’s surface,” said Colin Mitchell, a Cassini imaging team associate at the Space Science Institute in Boulder, Colorado, and lead author of the paper.

Mitchell and his colleagues created computer simulations to trace the tendrils back to outbursts from individual geysers on Enceladus, based on actual Cassini data.

FACT: To date, 101 individual active geysers have been identified on Enceladus. Source

Enceladus' jets feed the diffuse E ring

Enceladus’ icy jets feed the diffuse E ring around Saturn (NASA/JPL/SSI)

The researchers found the tendrils are composed of particles with diameters no smaller than about a millionth of a meter (one micrometer, or micron), which is consistent with the measurements of E-ring particles made by other Cassini instruments.

These icy particles are extremely fine; for a sense of scale, the smallest individual speck of dust our eyes can make out is about 50 microns in diameter.

Determining the rate of ice insertion into the E ring and the mass of what’s already there will help scientists figure out how much water is inside Enceladus, how much there was, and how long it might have been there.

“As the supply lanes for Saturn’s E ring, the tendrils give us a way to ascertain how much mass is leaving Enceladus and making its way into Saturn orbit,” said Carolyn Porco, Cassini imaging team leader and a coauthor on the paper. “So, another important step is to determine how much mass is involved, and thus estimate how much longer the moon’s sub-surface ocean may last.”

Read more on the Cassini mission site here.

Source: NASA/JPL


About Jason Major

Jason is a Rhode Island-based graphic designer, photographer, nature lover, space exploration fanatic, and coffee addict. In no particular order.

Posted on April 29, 2015, in Moons, Saturn's Moons and tagged , , , , , , , , , . Bookmark the permalink. 2 Comments.

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