  Current models of the solar wind must approximate (or ignore) the small-scale
dynamics within the solar atmosphere, however these are likely important in
shaping the emerging wave-turbulence spectrum and ultimately
heating/accelerating the coronal plasma. The Bifrost code produces realistic
simulations of the solar atmosphere that facilitate the analysis of spatial and
temporal scales which are currently at, or beyond, the limit of modern solar
telescopes. For this study, the Bifrost simulation is configured to represent
the solar atmosphere in a coronal hole region, from which the fast solar wind
emerges. The simulation extends from the upper-convection zone (2.5 Mm below
the photosphere) to the low-corona (14.5 Mm above the photosphere), with a
horizontal extent of 24 Mm x 24 Mm. The twisting of the coronal magnetic field
by photospheric flows, efficiently injects energy into the low-corona. Poynting
fluxes of up to $2-4$ kWm$^{-2}$ are commonly observed inside twisted magnetic
structures with diameters in the low-corona of 1 - 5 Mm. Torsional Alfv\'en
waves are favourably transmitted along these structures, and will subsequently
escape into the solar wind. However, reflections of these waves from the upper
boundary condition make it difficult to unambiguously quantify the emerging
Alfv\'en wave-energy flux. This study represents a first step in quantifying
the conditions at the base of the solar wind using Bifrost simulations. It is
shown that the coronal magnetic field is readily braided and twisted by
photospheric flows. Temperature and density contrasts form between regions with
active stirring motions and those without. Stronger whirlpool-like flows in the
convection, concurrent with magnetic concentrations, launch torsional Alfv\'en
waves up through the magnetic funnel network, which are expected to enhance the
turbulent generation of magnetic switchbacks in the solar wind.
