Living With the Young Sun: First Results of HST-XMM Newton and TESS Coordinated Observations of Young Suns and Modeling of Their Coronae, Winds and Eruptive Events

The young magnetically active solar-like stars are efficient generators of ionizing radiation in the form of X-ray and extreme-UV (EUV) flux, stellar winds, and eruptive events. The eruptive events include (super)flares with energies 100 times greater than that observed on the Sun. These outputs represent the critical factors affecting atmospheric escape and chemistry of (exo)planets around active stars. While X-ray fluxes and surface magnetic fields can be derived from observations, the EUV emission, and wind mass fluxes, coronal mass ejections and associated stellar energetic particle events cannot be directly observed, and thus remain elusive. Here, we present a new data constrained Star-as-The-Sun modeling approach as a viable way to reconstruct the coronal and wind environments of these stars. This approach is based on the results of our coordinated international multi-observatory "Evolving Magnetic Lives of Young Suns" that incorporates the data of four young solar-like stars, k1 Ceti, BE Ceti, eps Eri and V993 Tau. The derived HST data and stellar magnetograms retrieved from spectropolarimetry observations are used to constrain the Poynting flux via Alfven waves at the lower computational boundary of the three-dimensional magnetohydrodynamic model, Alfven Wave Solar Model (AWSoM). We present the results of 3D MHD simulations of stellar coronae and winds from young suns and show how the modeled background coronal environments are used to set the conditions for initiation and propagation of stellar coronal mass ejections and associated stellar energetic particle events.