General trends of stellar wind velocity (v_wind), coronal temperature (T_co), and wind’s mass-loss rate (﹩\dot{M}﹩), with respect to the effective temperature (T_eff) and Alfvén wave luminosity on the photosphere (L_A,ph), which is predicted by our semi-empirical method. The open circles in this figure represent part of the samples in our parameter survey. The thick dashed line corresponds to the fiducial L_A,ph as a function of T_eff. The thick dashed–dotted line corresponds to the largest L_A,ph obtained by assuming that the convective velocity reaches the sound speed on the photosphere. The thin dashed line represents L_A,ph as a function of T_eff, which results in v_wind = v_esc⋆.