Thermal Equilibrium States of Europa's Ice Shell: Implications for Internal Ocean Thickness and Surface Heat Flow

By H. Hussmann, Tilman Spohn, K. Wieczerkowski. 2002

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Empirical constraints on the salinity of the europan ocean and implications for a thin ice shell (2007, unknown): “Thermal-orbital evolution models support this possibility (Hussmann and Spohn, 2004; Hussmann et al., 2002).”
Tidal dissipation within large icy satellites: Applications to Europa and Titan (2005, unknown): “(2)] (e.g.,Peale et al., 1979; Fischer and Spohn, 19 Showman et al., 1997; Hussmann et al., 2002; Moore, 2 Sohl et al., 2003).”
Oceans in the icy Galilean satellites of Jupiter (2002, background): “Hussmann et al. (2002) have shown that tidal heating in such an ice shell can keep a subsurface europan ocean from freezing.”
Interior composition, structure and dynamics of the Galilean satellites (2004, methodology): “Hussmann et al. (2002) have calculated tidal heating rates in Europa’s ice shell and have searched for equilibrium between the tidal heating and heat transfer rates, both of which are functions of the ice shell thickness and the ice rheology.”
Tidally heated convection: Constraints on Europa's ice shell thickness (2003, methodology): “This has 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].”