Causal relations among the varying v_wind, T_co, ﹩\dot{M}﹩, ﹩{p}_{\mathrm{tr}}﹩, and ρ_co with respect to decreases in ﹩{L}_{{\rm{A}},\mathrm{ph}}/(4\pi {r}_{\star }^{2})﹩ and r_⋆(T_eff). Here ﹩{L}_{{\rm{A}},\mathrm{ph}}/(4\pi {r}_{\star }^{2})﹩ and r_⋆(T_eff) correspond to the vertical and horizontal axes of panels in Figure 18, respectively. The thick arrows depict the results of energy partitioning from L_A,ph to L_c,co or L_kin,wind. In particular, the decrease in ﹩{L}_{{\rm{A}},\mathrm{ph}}/(4\pi {r}_{\star }^{2})﹩ causes cooler T_co, faster v_wind, and smaller ﹩\dot{M}/(4\pi {r}_{\star }^{2})﹩. How these energy conversion efficiencies are determined is beyond the scope of the present study, but we mention that the energy conversion efficiency from L_A,co to L_kin,wind (α_wind/A) is independent of stars, chromospheric magnetic field strengths, and energy inputs from the photosphere (Section 5.2). Here α_wind/A is possibly dependent on the filling factor of the open flux tube (Appendix A).