Root mean square (RMS) values of radial (top panels) and tangential velocity perturbations (bottom panels) are shown for selected magnetic models as a function of radiation temperature, focusing on the (sub-)surface atmospheric layers before the onset of the stellar wind. The left column illustrates the results for a radial magnetic field configuration, while the right column corresponds to a horizontal magnetic field configuration. It is evident that a strong radial magnetic field suppresses horizontal gas motion, while a strong horizontal magnetic field inhibits radial gas movement. Notably, in the strongest field cases (20 kG), the tangential velocity perturbations approach or fall below 1 km/s.