The Wrinkles of Youth

Water Volcanoes

saturn_moon_family
Close view of Saturn’s moon, Enceladus. Click for larger view. A combination of spectral filters sensitive to infrared and polarized light was used to obtain this view. Resolution in the original image was about 2 kilometers (1.2 miles) per pixel. The image has been contrast-enhanced and magnified by a factor of two to aid visibility.
Credit: NASA/JPL

This Cassini image [right] of Saturn’s moon Enceladus shows a region containing bizarre, wrinkled terrain.

Enceladus is covered with bright water ice. The part of its surface visible here appears to be largely free of craters — indicating that it is geologically young.

The first close imaging of this moon will be done by Cassini in February 2005 and should reveal many surprises. Enceladus has a diameter of 499 kilometers (310 miles).

This view shows primarily the leading hemisphere of Enceladus. The image has been rotated so that north on Enceladus is up.

The image was acquired with the Cassini spacecraft narrow angle camera on Jan. 15, 2005, at a distance of approximately 367,000 kilometers (228,000 miles) from Enceladus and at a Sun-Enceladus-spacecraft, or phase, angle of 74 degrees.

According to the standard view of Enceladus: ‘At least five different types of terrain have been identified on Enceladus. In addition to craters there are smooth plains and extensive linear cracks and ridges. At least some of the surface is relatively young, probably less than 100 million years. This means that Enceladus must have been active until very recently (and perhaps is still active today). Perhaps some sort of "water volcanism" is at work. ‘

‘Enceladus is much too small to be heated by the decay of radioactive material in its interior at present (the heat would have all dissipated long ago). Enceladus is locked in a 1:2 resonance with Dione (similar to the situation between Io and Europa). This may provide a heating mechanism but it is probably insufficient to melt water ice. Enceladus may therefore be composed of some low-melting point material rather than pure water.’

Condensed ices give many of Saturn’s moons very high albedo (reflection coefficients) but some are mottled with darker regions that may be rich in organic chemicals like methane or ammonia. These building blocks for primitive biochemistry may offer insight into how a similar, but much warmer environment on Earth, might have given rise to primordial life.

Cassini will make close flybys of Enceladus, Hyperion, Dione and Rhea during a grand lunar tour.

enceladus
Saturn’s moon Enceladus.
Image Credit: NASA/JPL

Cassini is conducting a four-year orbital mission, circling Saturn 77 times and cruising by more than 50 close encounters (and another dozen or so more-distant encounters) with the planet’s moons. In all, Cassini will aim its instruments at 8 of Saturn’s 33 or more known moons. Cassini has already discovered a few that were unknown from ground observation and an earlier Voyager flyby.

"One of our major objectives in returning to Saturn was to survey the entire system for new bodies," said Dr. Carolyn Porco, imaging team leader, Space Science Institute, Boulder, Colo. "It’s really gratifying to know that among all the other fantastic discoveries we will make over the next four years, we can now add the confirmation of two new moons, unnoticed around Saturn for billions of years until now," she added.

Moons surrounding the giant planets generally are not found where they originally formed because tidal forces from the planet can cause them to drift from their original locations. In drifting, they may sweep through locations where other moons disturb them, making their orbits eccentric or inclined relative to the planet’s equator.


Related Web Pages

Cassini
Saturn Edition, Astrobiology Magaz.
Saturn’s Rings in UV
Cassini Closes In on Saturn

Saturn– JPL Cassini Main Page
Lord of the Rings
Space Science Institute, Imaging Team Boulder, Colorado
Saturn: The Closest Pass
Prebiotic Laboratory
Planet Wannabe
Where is Cassini Now?