  We analyse the most powerful X-ray outbursts from neutron stars in ten
Magellanic high-mass X-ray binaries and three pulsating ultraluminous X-ray
sources. Most of the outbursts rise to $L_{max}$ which is about the level of
the Eddington luminosity, while the rest and more powerful outbursts also
appear to recognize that limit when their emissions are assumed to be
anisotropic and beamed toward our direction. We use the measurements of pulsar
spin periods $P_S$ and their derivatives $\dot{P_S}$ to calculate the X-ray
luminosities $L_p$ in their faintest accreting ("propeller") states. In four
cases 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 the
ratios $L_p/L_{max}$ and we obtain an outstanding confluence of theory and
observations from which we conclude that work done on both fronts is accurate
and the results are trustworthy: sources known to reside on the lowest
Magellanic propeller line are all located on/near that line, whereas other
sources jump higher and reach higher-lying propeller lines. These jumps can be
interpreted in only one way, higher-lying pulsars have stronger surface
magnetic fields in agreement with empirical results in which $\dot{P_S}$ and
$L_p$ values were not used.
