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We analyse the most powerful X-ray outbursts from neutron stars in tenMagellanic high-mass X-ray binaries and three pulsating ultraluminous X-raysources. Most of the outbursts rise to $L_{max}$ which is about the level ofthe Eddington luminosity, while the rest and more powerful outbursts alsoappear to recognize that limit when their emissions are assumed to beanisotropic and beamed toward our direction. We use the measurements of pulsarspin periods $P_S$ and their derivatives $\dot{P_S}$ to calculate the X-rayluminosities $L_p$ in their faintest accreting ("propeller") states. In fourcases with unknown $\dot{P_S}$, we use the lowest observed X-ray luminosities,which only adds to the heterogeneity of the sample. Then we calculate theratios $L_p/L_{max}$ and we obtain an outstanding confluence of theory andobservations from which we conclude that work done on both fronts is accurateand the results are trustworthy: sources known to reside on the lowestMagellanic propeller line are all located on/near that line, whereas othersources jump higher and reach higher-lying propeller lines. These jumps can beinterpreted in only one way, higher-lying pulsars have stronger surfacemagnetic fields in agreement with empirical results in which $\dot{P_S}$ and$L_p$ values were not used.

A Striking Confluence Between Theory and Observations of High-Mass X-ray Binary Pulsars