Sarandib Planitia

Lore & Background

From Voyager images, Sarandib Planitia was considered part of either the ridged plains unit (Kargel and Pozio 1996) or smooth plains unit (Rothery 1999) of Enceladus, thought to be the youngest terrain on Enceladus. In more recent (and higher resolution) Cassini images, Sarandib is resolved into a region of relatively low ridges, with a band of rifted terrain cutting through the middle from northwest to southeast. A series of long-wavelength compression ridges are seen in the western portion, reminiscent of banded terrain on Europa, like Astypalaea Linea.

Sarandib Planitia is bounded on the north and west by a band of grooved terrain named Samarkand Sulci. Given the similarity in the spatial relationship between the Diyar Planitia and Harran Sulci, it is likely that the formation of Sarandib Planitia and Samarkand Sulci are related. Only approximately 20 craters larger than 1 kilometer across (the largest only 4.5 kilometers across) have been found in Sarandib, demonstrating the youthful age of the region.

Sarandib Planitia is named from the old Arabic/Persian/Urdu name for Sri Lanka, an island visited by Sindbad on his 6th voyage in Arabian Nights.

Reader's Guide

Sarandib Planitia holds significance as a key region for understanding the geological youth and tectonic activity of Enceladus. Its sparse crater population—only about 20 craters larger than 1 km across, with the largest at 4.5 km—directly demonstrates that this terrain is the youngest on the moon. The presence of low ridges, a rifted band cutting northwest to southeast, and long-wavelength compression ridges in the west suggests a complex tectonic history, with features analogous to banded terrain on Europa (e.g., Astypalaea Linea). The spatial relationship with Samarkand Sulci, a grooved band to the north and west, implies a genetic link between the planitia and the sulci, similar to the relationship between Diyar Planitia and Harran Sulci. The region's classification remains disputed between the ridged plains unit (Kargel and Pozio 1996) and smooth plains unit (Rothery 1999), reflecting ongoing uncertainty about its precise geological nature. Its legacy lies in providing a window into Enceladus's most recent surface processes, as revealed by both Voyager and Cassini imagery.