Termální vývoj Saturnova měsíce Enceladu

Kozoň, Marek

We study thermal evolution of Enceladus on very long time scales. In order to do so, we created a Fortran program modeling tidal deformation and thus induced heat dissipation as well as conductive transport of the heat in the body of the moon. Effect of long-lived radioactive isotopes decay in the core on the heat generation is included. We show the dependence of a thermal scenario character on different minimal viscosity and constant eccentricity values and study chosen cases in detail. We further demonstrate that, if orbital eccentricity evolution is incorporated, its initial value has no essential effect on the thermal evolution result, with the body always freezing quickly. Lastly, we examine the dependence of a thermal scenario on added values of hydrothermal heating power from the core and present that a power magnitude can be found, with which the satellite does not freeze, nor overheats in the first 4 billions of years what is necessary for maintaining a thermal activity on Enceladus since its formation to the present time. 1

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