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Over the south pole of Enceladus, an icy moon of Saturn, geysers eject waterinto space in a striped pattern, making Enceladus one of the most attractivedestinations in the search for extraterrestrial life. We explore the oceandynamics and tracer/heat transport associated with geysers as a function of theassumed salinity of the ocean and various core-shell heat partitions and bottomheating patterns. We find that, even if heating is concentrated into a narrowband on the seafloor directly beneath the south pole, the warm fluid becomesquickly mixed with its surroundings due to baroclinic instability. The warmingsignal beneath the ice is diffuse and insufficient to prevent the geyser fromfreezing over. Instead, if heating is assumed to be local to the geyser,emanating from tidal dissipation in the ice itself, the geyser can besustained. In this case, the upper ocean beneath the ice becomes stablystratified and thus a barrier to vertical communication, leading to transittimescales from the core to the ice shell of hundreds of years.

Dynamics or Geysers and tracer transport over the south pole of Enceladus