Jorick S. Vink, Gautham N. Sabhahit, Andreas A. C. Sander

The bi-stability jump is a long-standing theoretical prediction of radiatively driven wind theory, associated with Fe IV/III recombination around T = 21000 - 25000 K. While most theoretical approaches predict a strong increase in mass-loss rates across the bi-stability jump, most empirical mass-loss studies of OB supergiants have not revealed the expected signature. We computed new hydro-dynamically consistent PoWR models at low and intermediate Eddington parameters to test whether the bi-stability jump persists in the canonical B supergiant regime. The PoWR models presented here predict a robust bi-stability jump, with an increase in mass-loss rate by more than an order of magnitude and a simultaneous drop in terminal wind velocity in line with Monte Carlo models and other co moving frame (CMF) calculations. The jump coincides with a transition in the dominant line driver from Fe IV to Fe III. The presence of the bi-stability jump is not restricted to high Gammae objects and remains present for models well below the LBV/hypergiant regime. The persistence of the bi-stability jump in hydro-dynamically consistent models at lower Gammae supports the interpretation of the bi-stability jump as a temperature-driven ionisation effect that operates once a stationary line-driven wind solution exists. The continuing discrepancy between predictions and empirical population studies motivates further code comparison work and controlled observational tests using individual objects such as LBVs.