THE ACTIVE SOUTH POLAR TERRAIN OF ENCELADUS: HOW ITS JETS, HEAT AND TIDAL STRESSES ARE RELATED

In 2005, the Cassini mission at Saturn discovered a remarkable and unique geological province at the south pole of the small moon, Enceladus. Towering jets of powder-sized icy particles, and water vapor laced with organic compounds, vent from several prominent fractures crossing the 500-km wide south polar cap. And a shocking 16GW of thermal radiaion emitted by the region, among other lines of evidence, points to a regional sea below the south polar terrain, almost certainly created by the dissipation of tidal energy arising from a 2:1 orbital resonance between Enceladus and its sister moon, Dione. With excess heat, organics, and liquid water, the significance of this moon as a possible host of prebiotic chemistry, or even extraterrestrial organisms, is obvious.

This presentation will begin with a brief background on Cassini's findings at Enceladus and then examine the relationships between the jets, anomalous heat, and tidal stresses, and what these relationships mean for the mechanisms responsible for this moon's surprising activity.