Numerical simulations of wave excitation in magnetic flux tubes present are very distinct from idealized theoretical models. Unlike analytic studies with simplified boundary conditions and sharp interfaces, numerical MHD modelling must account for grid resolution, smoothing layers, and numerical noise. These are factors critical for producing results that are compatible with real solar observations. This work examines the fundamental methods and strategies employed in flux tube simulations, including a comparative analysis of numerical grids and the development of effective velocity drivers. Practical implementation coding techniques for MHD solvers are also provided, offering insights valuable for both new and experienced researchers.