Observational evidence has shown that waves are ubiquitous in the solar corona. As such, the role of wave-based heating mechanisms is attracting increased attention. In particular, phase mixing of Alfvén waves has been proposed as a possible mechanism to accelerate the dissipation of wave energy.

Using MHD simulations, we consider a 2D magnetic strand in hydrostatic equilibrium as a model for a coronal loop, and we investigate chromospheric evaporation due to heating by phase mixing of Alfvén waves. We implement a continuous, sinusoidal driver that generates propagating Alfvén waves along the loop. Due to the non-uniform density profile, these Alfvén waves dissipate through phase mixing and increase the temperature in the boundary of the loop. In this study, we investigate whether this leads to chromospheric evaporation and whether the subsequent change in the local coronal density is sufficient to alter the phase mixing process.