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This artist's rendering shows a regional cross-section of the ice shell underlying Enceladus' south polar terrain, illustrating our current knowledge of the physical and thermal structure and processes ongoing below and at the surface. Narrow cracks extend upward from the sub-surface sea all the way to the surface, through both ductile and brittle layers of the ice shell. Liquid water under pressure fills the cracks, keeping them open even through the ductile layer and providing a conduit for vapor and sea water to reach the near-surface. Other processes, such as volatile exsolution of gases, can drive vapor and water droplets all the way to the surface, forming geysers and condensing close to the surface, depositing latent heat. This heat is observed by Cassini's long-wavelength infrared instruments as the small-scale hot spots (dozens of feet, or tens of meters in size) surrounding each geyser (see PIA17189).
The subsurface regions immediately surrounding the sea and the cracks bearing water and vapor are expected to be warm. Regional heating from tidal flexing is also expected to be present, but is so far undetected.
The ice shell lying above the sea is comparable in thickness to the distance between the tiger stripe fractures, suggesting that the latter might be cracks formed in the past when tensional stresses across the region were stronger.
The surface area of the south polar terrain is approximately that of Scotland.
The Cassini Solstice Mission is a joint United States and European endeavor. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The imaging team consists of scientists from the US, England, France, and Germany. The imaging operations center and team lead (Dr. C. Porco) are based at the Space Science Institute in Boulder, Colo.