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Alfv\'enic fluctuations of various scales are ubiquitous in the corona; theirnon-linear interactions and eventual turbulent cascade result in an importantheating mechanism that accelerates the solar wind. These fluctuations may beprocessed by large-scale, transient, and coherent heliospheric structures suchas coronal mass ejections (CMEs). In this study we investigate the interactionsbetween Alfv\'enic solar wind fluctuations and CMEs using magnetohydrodynamic(MHD) simulations. We study the transmission of upstream solar windfluctuations into the CME leading to the formation of CME sheath fluctuations.Additionally, we investigate the influence of the fluctuation frequencies onthe extent of the CME sheath. We used an ideal MHD model with an adiabaticequation of state. An Alfv\'en pump wave is injected into the quiet solar windby perturbing the transverse magnetic field and velocity components, and a CMEis injected by inserting a flux-rope modelled as a magnetic island into thequasi-steady solar wind. The upstream Alfv\'en waves experience a decrease inwavelength and change in the wave vector direction due to the non-radialtopology of the CME shock front. The CME sheath inhibits the transmission oflong-wavelength fluctuations due to the presence of non-radial flows in thisregion. The frequency of the solar wind fluctuations also affects thesteepening of MHD fast waves causing the CME shock propagation speed to varywith the solar wind fluctuation frequencies.

Modelling the interaction of Alfv\'enic fluctuations with coronal mass ejections in the low solar corona