Since the first HI observations of the Milky Way warp 50 years ago numerous hypotheses have been proposed to explain this common galactic phenomenon. While actually most of the works on warps are based on the assumption of a disk embedded in a dark matter halo, the possibility of a heavy self-gravitating disk is often neglected. The aim of this paper is to better understand the constraints imposed by the shape of the dark component on the dynamics of the warp. Two set of simulations have been performed. The first one is based on a traditional dark matter halo, while the second one uses a heavy flaring self-gravitating disk.