Solar prominences are sheets of relatively cool and dense plasma which extend into the corona and have their feet within the photosphere. Forming in filament channels above polarity inversion lines found in the photosphere, prominences are magnetically suspended flux ropes. The origins of twist in prominence structures are investigated through modelling the inflow of plasma material during their formation, and considering the impact of torsional Alfvén waves which are ubiquitous to the system.

As a first step in this investigation, the linear domain has been considered in order to ascertain the conditions under which any potential twisting might be amplified within the system. This is achieved through analysis within which a flux tube is adopted with a time-dependent inflow, whilst equations of motion and induction are combined to describe the evolution of small scale linear twists experiencing magnetic perturbations. Analytical solutions are derived in terms of the hypergeometric function, which allow us to investigate the growth of the perturbations.

Finally, a numerical approach is adopted and compared with the analytical approach. For the numerical analysis, the governing equations are solved for given initial conditions that replicate a small amplitude torsional Alfvenic pulse. The evolution of the pulse for given initial and boundary conditions is investigated over time within the simulated prominence flux rope to explore the conditions in which an expected twisted structure can evolve.