We present current results from a project aiming to clarify how stellar winds evolve during the first billion years of the main sequence evolution of solar-type stars, and the implications for early solar evolution. This project is based on the extensive TOUPIES survey of stellar magnetic fields, with surface radial field maps used to model stellar winds via Space Weather Modelling Framework codes. We also explore numerical methods for producing wind models verifiable through direct comparisons with observations of the modern-day Sun. We find that a modelling approach used with solar magnetograms can be efficiently extended to survey a range of young solar-type stars with magnetic field strengths up to two orders of magnitude greater, but with some caveats regarding the assumptions needed and the interpretations gained from solar as well as stellar models. In our preliminary models wind mass loss does not exceed 1010 kg/s.

{"references": ["Folsom C. P., et al., 2016, MNRAS, 457, 580", "Folsom C. P., et al., 2018, MNRAS, 474, 4956"]}