Clues to the formation of Enceladus' south-polar terrain from simulations of funiscular plains formation

Cassini imaging and thermal data have demonstrated that Enceladus' four south-polar linear-fractures are the source of both Enceladus' cryovolcanic plume and its extreme thermal emission. These long (130 km), parallel 'tiger stripes' are located within a young, quasi-circular, south-polar depression characterized by extensive tectonic deformation that includes sets of both small-scale fractures (possibly relic tiger stripes) [Patthoff and Kattenhorn 2011], and large-amplitude circumferential ridges. Between the tiger stripes themselves are broad regions of periodic, low amplitude (50-100 m), short-wavelength (1 km) ridges (dubbed 'funiscular' terrain) that generally run parallel to the larger tiger stripe fractures but occasionally intersect them at small angles [Spencer et al. 2009]. The formation of the south polar terrain (SPT) may be related to localized melting of Enceladus' ice layer [e.g., Collins and Goodman, 2007] but the detailed formation kinematics of the SPT and its specific tectonic structures is far from certain. Here we constrain the formation of the SPT by simulating the development of funiscular terrain specifically. This terrain dominates the central portion of the SPT, including regions immediately adjacent to the tiger stripes. The stripes are, in effect, large-scale fractures imbedded within the funiscular terrain; thus, any kinematic or dynamic prescription for SPT formation must account for funiscular morphology. The simplest formation mechanism consistent with the funiscular ridges is that of low-amplitude, short-wavelength folding of a thin surface layer. Barr and Pruess [2010] demonstrated the plausibility of this mechanism using an analytical model developed for folds forming on lava flow tops. We extend their analysis using finite element modeling of the contraction of a thin, brittle lithosphere overlying ductile ice. We find fold morphologies consistent with the funiscular terrain (50-100 m amplitude, 1.5 km wavelengths) for lithospheric thicknesses of 250-500 m assuming weak (~100 kPa) near surface ice and 10% shortening. Creation of short wavelengths and tight fold hinges requires kinematic fold growth that shortens the fold wavelength subsequent to establishment of a longer, initial dominant wavelength. Thicker lithospheres (1 km) also reproduce the deformation if strains exceed 10%, though fold amplitudes are lower and wavelengths longer in this case. The thin lithosphere required to produce funiscular morphologies require exceedingly high heat flow if intact (low porosity) ice is assumed (≥1 W m^-2). Significant lithospheric porosity that depresses the ice thermal conductivity (e.g., by a factor of ~3 for 30% porosity [Shoshany et al. 2002]) is likely required, and could decrease the necessary heat flux to ~300 mW m^-2. The thin lithosphere necessary for its formation might account for the funiscular terrain's limited spatial extent adjacent to the tiger stripes, the locus of SPT thermal activity. A compressive stress regime between the tensile tiger stripes suggests local accommodation of strain in a dominantly extensional setting that is likely modulated by tidally-induced shear.