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Stars interact with their planets through gravitation, radiation, andmagnetic fields. Although magnetic activity decreases with time, reducingassociated high-energy (e.g., coronal XUV emission, flares), stellar windspersist throughout the entire evolution of the system. Their cumulative effectwill 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 windslook like and how they behave. Here we present the results from a grid of 3Dstate-of-the-art stellar wind models for cool stars (spectral types F to M). Weexplore the role played by the different stellar properties (mass, radius,rotation, magnetic field) on the characteristics of the resulting magnetizedwinds (mass and angular momentum losses, terminal speeds, wind topology) andisolate the most important dependencies between the parameters involved. Theseresults will be used to establish scaling laws that will complement the lack ofstellar wind observational constraints.

Quantification of the environment of cool stars using numerical simulations