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We present new wind models for {\tau} Bo\"otis ({\tau} Boo), ahot-Jupiter-host-star whose observable magnetic cycles makes it a uniquelyuseful target for our goal of monitoring the temporal variability of stellarwinds and their exoplanetary impacts. Using spectropolarimetric observationsfrom May 2009 to January 2015, the most extensive information of this type yetavailable, to reconstruct the stellar magnetic field, we produce multiple 3Dmagnetohydrodynamic stellar wind models. Our results show that characteristicchanges in the large-scale magnetic field as the star undergoes magnetic cyclesproduce changes in the wind properties, both globally and locally at theposition of the orbiting planet. Whilst the mass loss rate of the star variesby only a minimal amount ($\sim$ 4 percent), the rates of angular momentum lossand associated spin-down timescales are seen to vary widely (up to $\sim$ 140percent), findings consistent with and extending previous research. Inaddition, we find that temporal variation in the global wind is governed mainlyby changes in total magnetic flux rather than changes in wind plasmaproperties. The magnetic pressure varies with time and location and dominatesthe stellar wind pressure at the planetary orbit. By assuming a Jovianplanetary magnetic field for {\tau} Boo b, we nevertheless conclude that theplanetary magnetosphere can remain stable in size for all observed stellarcycle epochs, despite significant changes in the stellar field and theresulting local space weather environment.

Temporal variability of the wind from the star {\tau} Bo\"otis