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Current models of the solar wind must approximate (or ignore) the small-scaledynamics within the solar atmosphere, however these are likely important inshaping the emerging wave-turbulence spectrum and ultimatelyheating/accelerating the coronal plasma. The Bifrost code produces realisticsimulations of the solar atmosphere that facilitate the analysis of spatial andtemporal scales which are currently at, or beyond, the limit of modern solartelescopes. For this study, the Bifrost simulation is configured to representthe solar atmosphere in a coronal hole region, from which the fast solar windemerges. The simulation extends from the upper-convection zone (2.5 Mm belowthe photosphere) to the low-corona (14.5 Mm above the photosphere), with ahorizontal extent of 24 Mm x 24 Mm. The twisting of the coronal magnetic fieldby photospheric flows, efficiently injects energy into the low-corona. Poyntingfluxes of up to $2-4$ kWm$^{-2}$ are commonly observed inside twisted magneticstructures with diameters in the low-corona of 1 - 5 Mm. Torsional Alfv\'enwaves are favourably transmitted along these structures, and will subsequentlyescape into the solar wind. However, reflections of these waves from the upperboundary condition make it difficult to unambiguously quantify the emergingAlfv\'en wave-energy flux. This study represents a first step in quantifyingthe conditions at the base of the solar wind using Bifrost simulations. It isshown that the coronal magnetic field is readily braided and twisted byphotospheric flows. Temperature and density contrasts form between regions withactive stirring motions and those without. Stronger whirlpool-like flows in theconvection, concurrent with magnetic concentrations, launch torsional Alfv\'enwaves up through the magnetic funnel network, which are expected to enhance theturbulent generation of magnetic switchbacks in the solar wind.

Stirring the Base of the Solar Wind: On Heat Transfer and Vortex Formation