Same quantities as in Figure 4 for the simulation with penumbra and Evershed flow (see Figure 10 for an intensity snapshot and magnetogram from this simulation run). Differences compared to the previous case are restricted mostly to photospheric layers (see indicated τ = 0.1 level). While the previous case shows an inflow for R < 10 Mm and an outflow further out, radial flows are outward-directed for all distances in the presence of a penumbra. The large-scale outward-directed flow with amplitudes around 0.5 v _rms and the associated thermal perturbation are very similar to the previous case. Overall this points toward a large degree of independence of this flow component from the presence of a penumbra and Evershed flow.