DM and RM contribution from the clumpy stellar wind as the FRB progenitor moves behind the companion. The sudden changes in the DM and RM values are due to the clumps in the stellar wind. The vertical lines correspond to the jumps in DM and RM due to the clumps in the stellar wind. Different curves are shown for different inclinations of the orbit (0 corresponds to an edge-on orbit). The filling factor used for clumps for this simulation is 0.1.