Modeling the onset of solar eruptions in active regions

We present results of a numerical investigation into the initiation of solar coronal eruptions. Using numerical magnetohydrodynamic (MHD) models, we investigate the role of magnetic reconnection between emerging magnetic flux at the solar photosphere and pre-existing coronal flux in the eruptivity likelihood of emerging solar active regions. Our investigation covers a large range of spatial and temporal scales. We analyze the photospheric and coronal magnetic field to investigate how the relevant mechanisms that drive solar coronal eruptions can be detected by current and future observations.