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The nearby M dwarf WX UMa has recently been detected at radio wavelengthswith LOFAR. The combination of its observed brightness temperature and circularpolarisation fraction suggests that the emission is generated via theelectron-cyclotron maser instability. Two distinct mechanisms have beenproposed to power such emission from low-mass stars: either a sub-Alfv\'enicinteraction between the stellar magnetic field and an orbiting planet, orreconnection at the edge of the stellar magnetosphere. In this paper, weinvestigate the feasibility of both mechanisms, utilising the information aboutthe star's surrounding plasma environment obtained from modelling its stellarwind. Using this information, we show that a Neptune-sized exoplanet with amagnetic field strength of 10-100 G orbiting at ~0.034 au can accuratelyreproduce the observed radio emission from the star, with corresponding orbitalperiods of 7.4 days. Due to the stellar inclination, a planet in an equatorialorbit is unlikely to transit the star. While such a planet could induce radialvelocity semi-amplitudes from 7 to 396 m s$^{-1}$, it is unlikely that thissignal could be detected with current techniques due to the activity of thehost star. The application of our planet-induced radio emission model hereillustrates its exciting potential as a new tool for identifying planet-hostingcandidates from long-term radio monitoring. We also develop a model toinvestigate the reconnection-powered emission scenario. While this approachproduces less favourable results than the planet-induced scenario, itnevertheless serves as a potential alternative emission mechanism which isworth exploring further.

Radio masers on WX UMa: hints of a Neptune-sized planet, or magnetospheric reconnection?