  Stellar winds of cool, main-sequence stars are very tenuous and difficult to
observe. Despite carrying away only a small amount of the stellar mass, they
are important for regulating the rotation of the star and, consequently, its
activity and magnetism. As it permeates the interplanetary space, the stellar
wind interacts with any exoplanet encountered on its way, until it reaches the
interstellar medium (ISM). These interactions can result in complex physical
processes that depend on the characteristics of the wind. To better constrain
the wind characteristics, more realistic wind models that account for factors
such as stellar rotation and the complex/diverse observationally-derived
stellar magnetic field configurations of cool stars are required. In this
paper, I present a three-dimensional model of the wind of cool stars, which
adopt as boundary condition observationally-derived magnetic maps. I also
discuss how these studies are relevant for, e.g., the characterisation of the
interaction between stellar winds and planets/ISM, and the propagation of
cosmic rays.
