  Forming planets around young, fast-rotating solar-like stars are exposed to
an intense X-ray/extreme ultraviolet radiation field and strongly magnetized
stellar winds, as a consequence of the high magnetic activity of these stars.
Under these conditions, Earth-like exoplanets may experience a rapid loss of
their primordial hydrogen atmospheres, resulting in atmosphere-less rocky
obstacles for the stellar winds. The interaction of stellar winds with those
planets leads to the formation of potentially observable structures due to the
formation of large-scale magnetic field and density disturbances in the
vicinity of these planets, such as bow shocks, induced magnetospheres and
comet-like tails. In this work, we study the interaction between the stellar
winds of active, fast-rotating solar-like stars in the superfast-magnetosonic
regime with Earth-like, unmagnetized, tenuous atmosphere, planetary obstacles
through numerical 3D simulations using the PLUTO magnetohydrodynamical code.
The properties of AB Doradus, a nearby young star with a small rotation period
(0.51 days) and a strong flaring activity, have been used to parameterize this
early wind state. Bow shock and induced magnetosphere formation are
characterized through the alfv\'enic Mach number MA of the wind, for different
stellar wind configurations. Large bow shocks, up to an extension of ~7.0
planetary radii are found for low-MA winds. The general increase of density,
temperature and magnetic field in these large-scale structures formed around
planets may result in potentially detectable spectral signatures.
