Magnetic flux rope evolution and stability in data-driven coronal magnetic field simulations

Data-driven simulations of the solar corona have gathered traction in recent years for modelling the destabilisation of magnetic flux ropes (MFRs). To correctly apply and interpret results from these modelling efforts, it is crucial to understand how MFRs behave in such simulations and why they exhibit certain behaviour. For example, one aspect is to understand what effect does the evolution of the photospheric magnetic field have on the MFR system once it has reached an already unstable state. To probe the effect of data-driving, we first run a fully data-driven time-dependent magnetofrictional (TMF) simulation. Subsequently, we systematically relax the model (i.e., turn off the photospheric driving) at different times and analyse the MFRs' behaviour. In addition to the magnetofrictional relaxation, we also employ a zero-beta magnetohydrodynamics (MHD) model for the relaxation part of the analysis and compare the differences. To extract the simulated MFRs we use our novel Graphical User Interface for Tracking and Analysing flux Ropes (GUITAR). We find that even for MFRs that have been found to be eruptive in the relaxation simulations, MFR properties can greatly vary depending on the time of relaxation. Furthermore, there are striking differences between magnetofrictional and MHD relaxation simulations; not all initial TMF states which are eruptive in MHD are eruptive in the magnetofrictional relaxation. Furthermore, not only do the MFR properties significantly vary, but also the interpretation of which instability is at play varies between the two modelling prescriptions.