Thermal convection in the outer shell of large icy satellites

Details Thermal convection in the outer shell of large icy satellites Thermal convection in the outer shell of large icy satellites

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jgr...106.5107d&link_type=abstract

Journal of Geophysical Research, Volume 106, Issue E3, p. 5107-5121

Mathematics

Logic

33

Planetology: Solid Surface Planets: Interiors

Scientific paper

Evolution of large icy satellites is controlled by heat transfer across the outer ice I layer. After the core overturn a possible structure consists of a silicate core and a shell of molten ices. As the satellite cools down, the primordial ocean crystallizes. If the outer layer is thick enough, convection is very likely to occur in it. We have used the results of a recent two-dimensional numerical model of convection including variable viscosity to estimate the vigor and the efficiency of convection in this layer. Viscosity variations induce the apparition of a stagnant lid at the top of the fluid, which reduces the efficiency of heat transfer. In the present study, the Rayleigh number Ra and the heat flux Φ are computed as a function of the thickness of the layer, assuming that the ice flow is Newtonian. Calculations are first made for a generic satellite of radius R=2500km and mean density <ρ>=1.9g/cm3. It is then shown that variations of +/-500 km on the radius and +/-0.5 g/cm3 on the mean density do not induce significant differences in the values of Ra and Φ. On the other hand, variations of the reference viscosity μ0, and of the activation energy E induce major differences. The reference viscosity is equal to the viscosity close to the melting point, and its possible value yields around μ0=5×1013Pas. A possible value of E is 60 kJ/mol. For these values of the rheological parameters we find that the initial ocean may crystallize completely in ~3.6 Gyr. Higher values of μ0 and/or E reduce significantly the vigor and the efficiency of convection. The influence of the composition of the initial ocean is also investigated. The presence of ammonia reduces the convective strength and the heat flux. The upper structure of icy satellites is discussed as a function of the rheological and compositional parameters. The presence of a sub-surface ocean could be explained by either the presence of volatiles in the initial ocean or the presence of additional heat sources, such as tidal dissipation.

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