  The tidal deformations of a planet are often considered as markers of its
inner structure. In this work, we use the tide excitations induced by the Sun
on Venus for deciphering the nature of its internal layers. In using a Monte
Carlo Random Exploration of the space of parameters describing the thickness,
density and viscosity of 4 or 5 layer profiles, we were able to select models
that can reproduce the observed mass, total moment of inertia, $k_2$ Love
number and expected quality factor $Q$. Each model is assumed to have
homogeneous layers with constant density, viscosity and rigidity. These models
show significant contrasts in the viscosity between the upper mantle and the
lower mantle. They also rather favor a S-free core and a slightly hotter lower
mantle consistent with previous expectations.
