  The hot Jupiter HD189733b is expected to be a source of strong radio
emission, due to its close proximity to its magnetically active host star.
Here, we model the stellar wind of its host star, based on reconstructed
surface stellar magnetic field maps. We use the local stellar wind properties
at the planetary orbit obtained from our models to compute the expected radio
emission from the planet. Our findings show that the planet emits with a peak
flux density within the detection capabilities of LOFAR. However, due to
absorption by the stellar wind itself, this emission may be attenuated
significantly. We show that the best time to observe the system is when the
planet is near primary transit of the host star, as the attenuation from the
stellar wind is lowest in this region.
