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Magnetic B-stars often exhibit circularly polarized radio emission thought toarise from gyrosynchrotron emission by energetic electrons trapped in thecircumstellar magnetosphere. Recent empirical analyses show that the onset andstrength of the observed radio emission scale with both the magnetic fieldstrength and the stellar rotation rate. This challenges the existing paradigmthat the energetic electrons are accelerated in the current sheet betweenopposite-polarity field lines in the outer regions of magnetised stellar winds,which includes no role for stellar rotation. Building on recent success inexplaining a similar rotation-field dependence of H$\alpha$ line emission interms of a model in which magnetospheric density is regulated by centrifugalbreakout (CBO), we examine here the potential role of the associated CBO-drivenmagnetic reconnection in accelerating the electrons that emit the observedgyrosynchrotron radio. We show in particular that the theoretical scalings forenergy production by CBO reconnection match well the empirical trends forobserved radio luminosity, with a suitably small, nearly constant conversionefficiency $\epsilon \approx 10^{-8}$. We summarize the distinct advantages ofour CBO scalings over previous associations with an electromotive force, anddiscuss the potential implications of CBO processes for X-rays and otherobserved characteristics of rotating magnetic B-stars with centrifugalmagnetospheres.

Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars