  The cumulative effect of the magnetized stellar winds on exoplanets dominates
over other forms of star-planet interactions. When combined with
photoevaporation, these winds will lead to atmospheric erosion. This is
directly connected with the concept of Habitable Zone (HZ) planets around
late-type stars. Our knowledge of these magnetized winds is limited, making
numerical models useful tools to explore them. In this preliminary study, we
focus on solar-like stars exploring how different stellar wind properties scale
with one another. We used one of the most detailed physics-based models, the 3D
Alfv\'en Wave Solar Model part of the Space Weather ModelingFramework, and
applied it to the stellar winds domain. Our simulations showed that the
magnetic field topology on the star surface plays a fundamental role in shaping
the different stellar wind properties (wind speed, mass loss rate, angular
momentum loss rate). We conclude that a characterization of the Alfv\'en
surface is crucial when studying star-planet interaction as it can serve as an
inner-boundary of the HZ
