  BL and UV Ceti are a nearby (2.7 pc) binary system with similar masses,
spectral types, and rapid rotation rates, but very different magnetic activity.
UV Ceti's much stronger large-scale magnetic field may cause this difference,
highlighting key unanswered questions about dynamo processes in fully
convective objects. Here we present multi-epoch characterization of the radio
spectrum of UV Ceti spanning 1-105 GHz, exhibiting flared emission similar to
coronal activity, auroral-like emission analogous to planetary magnetospheres,
and slowly-varying persistent emission. Radio observations are a powerful means
to probe the role that the large-scale magnetic field of UV Ceti has in
non-thermal particle acceleration, because radio-frequency phenomena result
from both the activity of small-scale field features as well as large-scale
auroral current systems. We find temporal variability at all bands observed,
and a hint of rotational modulation in the degree of circular polarization up
to 40 GHz. The persistent component of the emission is fairly constant from
1-105 GHz, making optically thick emission or optically thin gyrosynchrotron
from electrons with an isotropic pitch angle distribution unlikely. We discuss
the possibility of emission mechanisms analogous to Jupiter's radiation belts.
