Top: empirical-maximum (Ṁ_max) and theoretical () wind performance numbers, η = Ṁ υ_∞/(L_*∕c), as a functionof T_eff, for our OB supergiants sub-sample, in the Geneva (magenta) and MESA (orange) approaches. Dashed and dotted-dashed lines correspond to theoretical predictions for a source with log L/L_⊙ = 5.75 and M_* = 45 M_⊙ for solar metallicity respectively based on Geneva and MESA implementations of V00 and V01. The shadowed regions represent the first (27.5–22.5 kK) and second (18.5–12.5 kK) bi-stability jump zones as defined by V00. Bottom: same as top panel, but showing theoretical wind performance numbers in the Geneva (magenta) and Fixed-jumps (light green) approaches, and a dotted-dashed line marking the theoretical model based on the Fixed-jumps implementation of V00 and V01. The shadowed region represents the first bi-stability jump zone (24.5–19.5 kK) for a central temperature of the jump of 22 kK. In both panels the early B-type Hypergiants in our sample are indicated with squares, whereas arrows indicate upper limits of Ṁ_max. Finally, arrows, dotted lines, and symbols as in Fig. 8.