Reconstructing the evolution of recurring coronal holes in space and time

Recurring Coronal Holes (CHs) are long-lived structures in the solar corosna that survive over multiple solar rotations. They are sources of open magnetic field and fast solar wind streams filling the interplanetary space. Of the recurring CHs, those that can generate geomagnetic activity are particularly important due to the recurring impact they can have on the terrestrial environment. In this study we focus on reconstructing their vertical structure and assess how that changes with each rotation. To facilitate our study, we utilized the Potential Field Source Surface (PFSS) and the Schatten Current Sheet (SCS) model incorporated in the coronal modelling domain of EUHFORIA (European Heliospheric Forecasting Information Asset). We investigate the optimal parameter space for model initiation for each CH, compare the model output both to EUV and coronagraph white-light emissions, and assess the reconstructed heliospheric conditions using in situ measurements from different positions throughout the inner heliosphere.