  The medium around massive stars is strongly shaped by the stellar winds.
Those winds depend on various stellar parameters (effective temperature,
luminosity, chemical composition, rotation, ...), which are varying as a
function of the time. Using the wind properties obtained by classical stellar
evolution code allows for the multi- D hydrodynamical simulation of the
circum-stellar medium accounting for the time variations of the wind. We
present here the preliminary results of the simulation of the medium around a
fast rotating star. Comparing the results of such simulations with the observed
properties of the circum-stellar medium will allow to better understand the
interactions of the stellar winds with the interstellar medium, and could give
hints on the past history of the mass loss around massive stars, providing
constraints for stellar models.
