  The impact of the inner structure and thermal history of planets on their
observable features, such as luminosity or magnetic field, crucially depends on
the poorly known heat and charge transport properties of their internal layers.
The thermal and electric conductivities of different phases of water (liquid,
solid, and super-ionic) occurring in the interior of ice giant planets, such as
Uranus or Neptune, are evaluated from equilibrium ab initio molecular dynamics,
leveraging recent progresses in the theory and data analysis of transport in
extended systems. The implications of our findings on the evolution models of
the ice giants are briefly discussed
