Test whether the assumed auroral-radio beaming pattern is incompatible with rho Oph C

Determine whether the tangent-plane or other assumed electron-cyclotron-maser-instability beaming pattern is physically incompatible with the nearly constant auroral radio emission observed from the highly inclined, low-obliquity magnetic B star rho Oph C.

Background

Models of the auroral radio emission from rho Oph C imply a very broad azimuthal beaming angle, which contrasts with expectations from tangent-plane beaming models. Refraction, alternative electron energy distributions, or detailed growth-rate calculations could potentially reconcile the observed phase coverage with a narrower or otherwise different radiation pattern. The paper leaves unresolved whether the adopted beaming geometry is fundamentally inappropriate for this high-inclination, low-obliquity system.