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We present stellar wind modelling of the hot Jupiter host HD189733, andpredict radio emission from the stellar wind and the planet, the latter arisingfrom the interaction of the stellar wind with the planetary magnetosphere. Ourstellar wind models incorporate surface stellar magnetic field maps at theepochs Jun/Jul 2013, Sep 2014, and Jul 2015 as boundary conditions. We findthat the mass-loss rate, angular momentum-loss rate, and open magnetic flux ofHD189733 vary by 9%, 40%, and 19% over these three epochs. Solving theequations of radiative transfer, we find that from 10 MHz-100 GHz the stellarwind emits fluxes in the range of $10^{-3}$-$5$ $\mu$Jy, and becomes opticallythin above 10 GHz. Our planetary radio emission model uses the radiometricBode's law, and neglects the presence of a planetary atmosphere. For assumedplanetary magnetic fields of 1-10 G, we estimate that the planet emits atfrequencies of 2-25 MHz, with peak flux densities of $\sim10^2$ mJy. We findthat the planet orbits through regions of the stellar wind that are opticallythick to the emitted frequency from the planet. As a result, unattenuatedplanetary radio emission can only propagate out of the system and reach theobserver for 67% of the orbit for a 10 G planetary field, corresponding to whenthe planet is approaching and leaving primary transit. We also find that theplasma frequency of the stellar wind is too high to allow propagation of theplanetary radio emission below 21 MHz. This means a planetary field of at least8 G is required to produce detectable radio emission.

MOVES II. Tuning in to the radio environment of HD189733b