X-ray binaries are excellent laboratories for understanding the accretion processes around compact objects. Despite being one of the most studied High-Mass X-ray binaries in our Universe, Cyg X-1 keeps exhibiting misunderstood behaviours. Simultaneous high-resolution optical spectroscopy and X-ray observations of the system show an anti-correlation between the X-ray flux from the accretion disk and the optical emission from the blue supergiant strong wind. Additionally, the Disentangling method enabled the separation of the spectral signature of the focused wind and the photospheric region. The spectra show the well-known H-alpha line and an additional He II emission line, broad and intense in the spectrum of the focused wind component. Not only dependent on the X-ray spectral state of the system, these lines seem to strongly depend on the orbital motion of the star, which could be explained by the formation of high-density clumps in the line of sight.