  The archetypical flare star UV Cet was observed by MeerKAT on 5-6 October
2021. A large radio outburst with a duration of $\sim\!2$ hr was observed
between 886-1682 MHz with a time resolution of 8s and a frequency resolution of
0.84 MHz, enabling sensitive dynamic spectra to be formed. The emission is
characterized by three peaks containing a multitude of broadband arcs or
partial arcs in the time-frequency domain. In general, the arcs are highly
right-hand circularly polarized. During end of the third peak, brief bursts
occur that are significantly elliptically polarized. We present a simple model
that appears to be broadly consistent with the characteristics of the radio
emission from UV Cet. Briefly, the stellar magnetic field is modeled as a
dipole aligned with the rotational axis of the star. The radio emission
mechanism is assumed to be due to the cyclotron maser instability where x-mode
radiation near the electron gyrofrequency is amplified. While the elliptically
polarized bursts may be intrinsic to the source, rather stringent limits are
imposed on the plasma density in the source and along the propagation path. We
suggest that the elliptically polarized radiation may instead be the result of
reflection on an over-dense plasma structure at some distance from the source.
Radio emission from UV~Cet shares both stellar and planetary attributes.
