  Stars interact with their planets through gravitation, radiation, and
magnetic fields. Although magnetic activity decreases with time, reducing
associated high-energy (e.g., coronal XUV emission, flares), stellar winds
persist throughout the entire evolution of the system. Their cumulative effect
will be dominant for both the star and for possible orbiting exoplanets,
affecting in this way the expected habitability conditions. However,
observations of stellar winds in low-mass main sequence stars are limited,
which motivates the usage of models as a pathway to explore how these winds
look like and how they behave. Here we present the results from a grid of 3D
state-of-the-art stellar wind models for cool stars (spectral types F to M). We
explore the role played by the different stellar properties (mass, radius,
rotation, magnetic field) on the characteristics of the resulting magnetized
winds (mass and angular momentum losses, terminal speeds, wind topology) and
isolate the most important dependencies between the parameters involved. These
results will be used to establish scaling laws that will complement the lack of
stellar wind observational constraints.
