MURaM simulations used in the analysis. Top: maps of vertical velocity V_z at the continuum optical-depth unity surface (τ_Ross = 1 surface) for the Sun (left), G9 (middle), and K4 (right). We define granules and intergranular lanes by the sign of the vertical velocity V_Z; granules have V_Z < 0 (upflows, toward the observer), and intergranular lanes have V_Z > 0 (downflows, away from the observer). Middle: horizontally averaged V_Z versus ﹩\mathrm{log}{\tau }_{{\rm{Ross}}}﹩ for granules (blue), intergranular lanes (red), and the entire simulated domain mean (black); shading shows the 1σ dispersion ﹩{\sigma }_{{V}_{Z}}﹩ (we define ﹩{\sigma }_{{V}_{z}}({\tau }_{{\rm{Ross}}})﹩ as the standard deviation of the vertical velocity V_z on the ﹩{\tau }_{{\rm{Ross}}}={\rm{const}}﹩ surface) of the vertical velocity. Bottom: horizontally averaged temperature profiles for granules (blue), intergranular lanes (red), and the entire simulated domain mean (black) versus ﹩\mathrm{log}{\tau }_{{\rm{Ross}}}﹩. For panels (d)–(k), averages at each ﹩\mathrm{log}{\tau }_{{\rm{Ross}}}﹩ are computed along the corresponding constant optical depth surface. Toward cooler spectral types, the granulation pattern persists but with reduced amplitude.