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We present the results of a comprehensive numerical simulation of theenvironment around three exoplanet-host stars (HD 1237, HD 22049, and HD147513). Our simulations consider one of the latest models currently used forspace weather studies in the Heliosphere. Large-scale magnetic field maps,recovered with two implementations of the tomographic technique ofZeeman-Doppler imaging, serve to drive steady-state solutions in each system.This paper contains the description of the stellar wind and inner astrosphere,while the coronal structure was previously discussed in Alvarado-G\'omez et al.(2016). The analysis includes the magneto-hydrodynamical properties of thestellar wind, the associated mass and angular momentum loss rates, as well asthe topology of the astrospheric current sheet in each system. A systematiccomparison among the considered cases is performed, including two referencesolar simulations covering activity minimum and maximum. For HD 1237, weinvestigate the interactions between the structure of the developed stellarwind, and a possible magnetosphere around the Jupiter-mass planet in thissystem. We find that the process of particle injection into the planetaryatmosphere is dominated by the density distribution rather than velocityprofile of the stellar wind. In this context, we predict a maximum exoplanetaryradio emission of 12 mJy at 40 MHz in this system, assuming the crossing of ahigh-density streamer during periastron passage. Furthermore, in combinationwith the analysis performed in Alvarado-G\'omez et al. (2016), we obtain forthe first time a fully simulated mass loss-activity relation, which is comparedand discussed in the context of the relation based on astrospheric detectionsproposed by Wood et al. (2005a). Finally, we provide a characterisation of the3D properties of the stellar wind of these systems, at the inner edges of theirhabitable zones.

Simulating the environment around planet-hosting stars - II. Stellar winds and inner astrospheres