  Tau Boo is an intriguing planet-host star that is believed to undergo
magnetic cycles similar to the Sun, but with a duration that is about one order
of magnitude smaller than that of the solar cycle. With the use of
observationally derived surface magnetic field maps, we simulate the magnetic
stellar wind of Tau Boo by means of three-dimensional MHD numerical
simulations. As the properties of the stellar wind depend on the particular
characteristics of the stellar magnetic field, we show that the wind varies
during the observed epochs of the cycle. Although the mass loss-rates we find
(~2.7e-12 Msun/yr) vary less than 3 per cent during the observed epochs of the
cycle, our derived angular momentum loss-rates vary from 1.1 to 2.2e32erg. The
spin-down times associated to magnetic braking range between 39 and 78Gyr. We
also compute the emission measure from the (quiescent) closed corona and show
that it remains approximately constant through these epochs at a value of
~10^{50.6} cm^{-3}. This suggests that a magnetic cycle of Tau Boo may not be
detected by X-ray observations. We further investigate the interaction between
the stellar wind and the planet by estimating radio emission from the
hot-Jupiter that orbits at 0.0462 au from Tau Boo. By adopting reasonable
hypotheses, we show that, for a planet with a magnetic field similar to Jupiter
(~14G at the pole), the radio flux is estimated to be about 0.5-1 mJy,
occurring at a frequency of 34MHz. If the planet is less magnetised (field
strengths roughly <4G), detection of radio emission from the ground is
unfeasible due to the Earth's ionospheric cutoff. According to our estimates,
if the planet is more magnetised than that and provided the emission beam
crosses the observer line-of-sight, detection of radio emission from Tau Boo b
is only possible by ground-based instruments with a noise level of < 1 mJy,
operating at low frequencies.
