The auroral emission we observe at the Earth is known to be powered by the solar wind. Using this analogy, we expect that stellar winds can power auroral emission in magnetised exoplanets. This emission peaks at the radio wavelengths of the electromagnetic spectrum. Here, I present our recent predictions of the radio emission from V830 Tau b, which we model as being powered by the stellar wind of its host star. V830 Tau is the youngest (2 Myr) detected exoplanet to date. Due to its youth, the host star wind is expected to be have high densities, which could also generate radio emission of its own. From our model, we also compute the emission from the host star and we show that V830 Tau b could orbit inside the radio-photosphere of host star's wind. In this case, the stellar wind might prevent emission of the exoplanet to escape, depending on the planetary magnetic field strength. Observing radio emission from this system, even if only to provide upper limits, will allow us to simultaneously characterise the physical conditions of the star's wind and of its exoplanet.