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Fast rotating Wolf-Rayet stars are expected to be progenitors of longduration gamma-ray bursts. However, the observational test of this model isproblematic. Spectral lines of Wolf-Rayet stars originate in expanding stellarwind, therefore a reliable spectroscopical determination of their rotationalvelocities is difficult. Intrinsic polarization of Wolf-Rayet stars due to therotational modulation of the stellar wind may provide an indirect way todetermine the rotational velocities of these stars. However, detailed windmodels are required for this purpose. We determine the intrinsic polarizationof Wolf-Rayet stars from hydrodynamical wind models as a function of rotationalvelocity. We used 2.5D hydrodynamical simulations to calculate the structure ofrotating winds of Wolf-Rayet stars. The simulations account for the deformationof the stellar surface due to rotation, gravity darkening, and nonradialforces. From the derived models, we calculated the intrinsic stellarpolarization. The mass loss rate was scaled to take realistic wind densities ofWolf-Rayet stars into account. The hydrodynamical wind models predict a prolatewind structure, which leads to a relatively low level of polarization. Evenrelatively large rotational velocities are allowed by observational constrains.The obtained wind structure is similiar to that obtained previously forrotating optically thin winds. Derived upper limits of rotational velocities ofstudied Wolf-Rayet stars are not in conflict with the model of long durationgamma-ray bursts

Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind