The first results of the STORMGENESIS project will be introduced in this presentation. This project aims to characterize the initiation, propagation and connectivity of solar storms using innovative and ambitious numerical simulations based on the PLUTO code combined with the latest space weather observations. In this presentation, I will focus on the first part of the project which is the characterisation of the eruptive properties of an active region. Considering that estimating the magnetic field above the photosphere is one of the big uncertainties for our understanding of solar eruptions, we use different extrapolation techniques (potential, non-linear force-free, and non-force-free fields) based on an HMI magnetogram. We study how these different configurations influence the dynamics of the magnetic structure when considered very close to the onset of the observed eruption and how the energy is repartitioned for each extrapolation strategy. We also reproduce synthetic EUV emission out of these models. This work takes us a step closer to understanding the eruptivity of a given AR, as well as the energy channelling during the eruption, and hence, it improves our predictive and forecasting abilities for space weather purposes.