  The nearby M dwarf WX UMa has recently been detected at radio wavelengths
with LOFAR. The combination of its observed brightness temperature and circular
polarisation fraction suggests that the emission is generated via the
electron-cyclotron maser instability. Two distinct mechanisms have been
proposed to power such emission from low-mass stars: either a sub-Alfv\'enic
interaction between the stellar magnetic field and an orbiting planet, or
reconnection at the edge of the stellar magnetosphere. In this paper, we
investigate the feasibility of both mechanisms, utilising the information about
the star's surrounding plasma environment obtained from modelling its stellar
wind. Using this information, we show that a Neptune-sized exoplanet with a
magnetic field strength of 10-100 G orbiting at ~0.034 au can accurately
reproduce the observed radio emission from the star, with corresponding orbital
periods of 7.4 days. Due to the stellar inclination, a planet in an equatorial
orbit is unlikely to transit the star. While such a planet could induce radial
velocity semi-amplitudes from 7 to 396 m s$^{-1}$, it is unlikely that this
signal could be detected with current techniques due to the activity of the
host star. The application of our planet-induced radio emission model here
illustrates its exciting potential as a new tool for identifying planet-hosting
candidates from long-term radio monitoring. We also develop a model to
investigate the reconnection-powered emission scenario. While this approach
produces less favourable results than the planet-induced scenario, it
nevertheless serves as a potential alternative emission mechanism which is
worth exploring further.
