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A small subset of Galactic O-stars possess surface magnetic fields that alterthe outflowing stellar wind by magnetically confining it. Key to the magneticconfinement is that it induces rotational modulation of spectral lines over thefull EM domain; this allows us to infer basic quantities, e.g., mass-loss rateand magnetic geometry. Here, we present an empirical study of the H$\alpha$line in Galactic magnetic O-stars to constrain the mass fed from the stellarbase into the magnetosphere, using realistic multi-dimensional magnetized windmodels, and compare with theoretical predictions. Our results suggest that itmay be reasonable to use mass-feeding rates from non-magnetic wind theory ifthe absolute mass-loss rate is scaled down according to the amount of windmaterial falling back upon the stellar surface. This provides then someempirical support to the proposal that such magnetic O-stars might evolve intoheavy stellar-mass black holes (Petit et al. 2017)

First Empirical Constraints on the Low H$\alpha$ Mass-Loss Rates of Magnetic O-Stars