  We report high-frequency pulsations in WR135 from short cadence optical
photometric and spectroscopic time series surveys. The harmonics up to $6^{th}$
order are detected from the integrated photometric flux variation while the
comparatively weaker $8^{th}$ harmonic is detected from the varying strengths
of the least blended emission lines. We investigate the atmospheric
stratification of the stellar winds of WR135 using a radiative transfer
modeling code, CMFGEN, and find the physical conditions that can support the
propagation of such pulsations. From our study, we find that the sub-sonic
layers of the atmosphere are close to the Eddington limit and are launched by
the Fe-opacity. While the outer optically thin super-sonic winds
($\tau_{ross}$=0.1-0.01) are driven by the He II and C IV opacities. The
stratified winds above the sonic point undergo velocity perturbation that can
lead to clumps. We find that the optically thin supersonic winds
($\tau_{ross}$=0.1-0.01) contain dense smaller clumps (f=0.2-0.3) that
oscillate under the higher-order harmonics of the pulsation. These clumps grow
larger (f=0.1), dominate the outer stellar winds ($\tau_{ross}$=0.01-0.001),
and oscillate under the lower-order harmonics.
