Oceans in the icy Galilean satellites of Jupiter

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Tidally heated convection: Constraints on Europa's ice shell thickness (2003, methodology): “been applied to the rate of cooling of an icy satellite [Grasset and Sotin, 1996; McKinnon, 1999; Deschamps and Sotin, 2001; Ruiz, 2001; Hussmann et al., 2002; Spohn and Schubert, 2003].”
JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter system (2013, background): “evolution (Spohn and Schubert, 2003), advocate the presence of liquid water oceans below the icy crust.”
Magnetospheric interactions with satellites (2004, background): “Models of the heat flow (Spohn and Schubert 2003) show that for reasonable assumptions regarding the temperature and pressure dependence of the viscosity, it is possible to account for a region of melt below the surface ice, and the characteristics of the icy surface make the presence of a sub-surfa”
Interior composition, structure and dynamics of the Galilean satellites (2004, methodology): “The thickness of the shell D that is in equilibrium with an assumed heat flow into the base of the ocean can then be calculated to be approximately (Spohn and Schubert 2003)”