Geophysical data from the Cassini spacecraft imply the presence of a global ocean underneath the ice shell of Enceladus1, only a few kilometres below the surface in the South Polar Terrain2,3,4. Chemical analyses indicate that the ocean is salty5 and is fed by ongoing hydrothermal activity6,7,8. In order to explain these observations, an abnormally high heat power (>20 billion watts) is required, as well as a mechanism to focus endogenic activity at the south pole9,10. Here, we show that more than 10 GW of heat can be generated by tidal friction inside the unconsolidated rocky core. Water transport in the tidally heated permeable core results in hot narrow upwellings with temperatures exceeding 363 K, characterized by powerful (1–5 GW) hotspots at the seafloor, particularly at the south pole. The release of heat in narrow regions favours intense interaction between water and rock, and the transport of hydrothermal products from the core to the plume sources. We are thus able to explain the main global characteristics of Enceladus: global ocean, strong dissipation, reduced ice-shell thickness at the south pole and seafloor activity. We predict that this endogenic activity can be sustained for tens of millions to billions of years.
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The research leading to these results received financial support from the CNRS PICS (G.C., G.T.), the CNRS-INSU PNP program (G.C., G.T.) and the ANR OASIS project (G.C., G.T.), from the Czech Science Foundation project 15-14263Y (OS), from the German Research Foundation DFG projects PO 1015/2-1, /3-1, /4-1 (F.P.) and from the Icy Worlds node of NASA’s Astrobiology Institute 13-NAI7-0024 (C.S.). The computations were carried out using CCIPL computational facilities (France).
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Tidal synchronization of close-in satellites and exoplanets. III. Tidal dissipation revisited and application to Enceladus
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