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We consider propagation of polarization in the inner parts of pair-symmetricmagnetar winds, close to the light cylinder. Pair plasmas in magnetic field isbirefringent, a $\propto B^2$ effect. As a result, such plasmas work as phaseretarders: Stokes parameters follow a circular trajectory on the Poincaresphere. In the highly magnetized regime, $\omega, \, \omega_p \ll \omega_B$,the corresponding rotation rates are independent of the magnetic field. Aplasma screen with dispersion measure DM $\sim 10^{-6}$ pc cm$^{-3}$ can inducelarge polarization changes, including large effective Rotation Measure (RM).The frequency scaling of the (generalized) RM, $ \propto \lambda ^\alpha $,mimics the conventional RM with $\alpha =2$ for small phase shifts, but can beas small as $\alpha =1$. In interpreting observations the frequency scaling ofpolarization parameters should be fitted independently. The model offersexplanations for (i) large circular polarization component observed in FRBs,with right-left switching; (ii) large RM, with possible sign changes; (iii)time-depend variable polarization. Relatively dense and slow wind is needed -the corresponding effect in regular pulsars is small.

Faraday conversion in pair-symmetric winds of magnetars and Fast Radio Bursts