Effective elastic thickness and heat flux estimates on Ganymede. Non-Newtonian topographic relaxation on Europa. Discrete alternating hotspot islands formed by interaction of magma transport and lithospheric flexure. The great thickness debate: ice shell thickness models for Europa and comparisons with estimates based on flexure at ridges. Structural mapping of Enceladus and implications for formation of tectonized regions. Cryoclastic origin of particles on the surface of Enceladus. Total particulate mass in Enceladus plumes and mass of Saturn’s E ring inferred from Cassini ISS images. Shear heating as the origin of the plumes and heat flux on Enceladus. In Lunar and Planetary Science XLVIII 1955 (LPI, 2017). Break the world’s shell: an impact on Enceladus: bringing the ocean to the surface. Diapir-induced reorientation of Saturn’s moon Enceladus. True polar wander of Enceladus from topographic data. Powering prolonged hydrothermal activity inside Enceladus. Viscoelastic relaxation of Enceladus’s ice shell. Interior thermal state of Enceladus inferred from the viscoelastic state of the ice shell. in Enceladus and the Icy Moons of Saturn (eds Schenk, P. Mechanics of evenly spaced strike-slip faults and its implications for the formation of tiger-stripe fractures on Saturn’s moon Enceladus. Gravitational spreading, bookshelf faulting, and tectonic evolution of the south polar terrain of Saturn’s moon Enceladus. Constraining the heat flux between Enceladus’ tiger stripes: numerical modeling of funiscular plains formation. A fracture history on Enceladus provides evidence for a global ocean. Enceladus’s measured physical libration requires a global subsurface ocean. The gravity field and interior structure of Enceladus. A salt-water reservoir as the source of a compositionally stratified plume on Enceladus. Postberg, F., Schmidt, J., Hillier, J., Kempf, S. Enceladus’s ice shell structure as a window on internal heat production. Fracture penetration in planetary ice shells. Pressurized oceans and the eruption of liquid water on Europa and Enceladus. Sustained eruptions on Enceladus explained by turbulent dissipation in tiger stripes. How the geysers, tidal stresses, and thermal emission across the south polar terrain of Enceladus are related. Cassini observes the active south pole of Enceladus. The sequence of fissures then cascades outwards until the loading becomes too weak or the background shell thickness becomes too great to permit through-going fractures. The steadily erupting water ice loads the flanks of the open fissure, causing bending in the surrounding elastic plate and further tensile failure in bands parallel to the first fracture-a process that may be unique to Enceladus, where the gravity is too weak for compressive stresses to prevent fracture propagation through the thin ice shell. The tensile stresses are thereby relieved, preventing a similar failure at the opposite pole. Here we propose that secular cooling, which leads to a thickening of the ice shell and building of global tensile stresses 5, 6, causes the first fracture to form at one of the poles, where the ice shell is thinnest owing to tidal heating 7. To date, no study simultaneously explains why the tiger stripes should be located only at the south pole, why there are multiple approximately parallel and regularly spaced fractures, what accounts for their spacing of about 35 km, and why similarly active fissures have not been observed on other icy bodies. Active eruptions from the south polar region of Saturn’s ~500-km-diameter moon Enceladus are concentrated along a series of lineaments known as the ‘tiger stripes’ 1, 2, thought to be partially open fissures that connect to the liquid water ocean beneath the ice shell 3, 4.
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