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Magnetic confinement of stellar winds leads to the formation ofmagnetospheres, which can be sculpted into Centrifugal Magnetospheres (CMs) byrotational support of the corotating plasma. The conditions required for theCMs of magnetic early B-type stars to yield detectable emission in H$\alpha$ --the principal diagnostic of these structures -- are poorly constrained. A keyreason is that no detailed study of the magnetic and rotational evolution ofthis population has yet been performed. Using newly determined rotationalperiods, modern magnetic measurements, and atmospheric parameters determinedvia spectroscopic modelling, we have derived fundamental parameters, dipolaroblique rotator models, and magnetospheric parameters for 56 early B-typestars. Comparison to magnetic A- and O-type stars shows that the range ofsurface magnetic field strength is essentially constant with stellar mass, butthat the unsigned surface magnetic flux increases with mass. Both the surfacemagnetic dipole strength and the total magnetic flux decrease with stellar age,with the rate of flux decay apparently increasing with stellar mass. We findtentative evidence that multipolar magnetic fields may decay more rapidly thandipoles. Rotational periods increase with stellar age, as expected for amagnetic braking scenario. Without exception, all stars with H$\alpha$ emissionoriginating in a CM are 1) rapid rotators, 2) strongly magnetic, and 3) young,with the latter property consistent with the observation that magnetic fieldsand rotation both decrease over time.

The Magnetic Early B-type Stars III: A main sequence magnetic, rotational, and magnetospheric biography