Speaker
Description
Modelling solar eruptions is crucial to understand their triggers and how they might impact Earth's magnetic environment. Thus, magnetic field simulations of the low solar corona are of great relevance for space weather forecasting. In particular, simulations that are driven by the observed magnetic field at the photosphere have proven to be a powerful tool to model the energy build up and destabilization of magnetic flux ropes (MFRs), leading to their eruption. However, especially for models that do not evolve on physical timescales, it is important to understand the effect of the photospheric driving on the MFR system. For example, at which point in the simulation does the system become unstable and what is the influence of the magnetogram evolution on the MFR once it has already reached an unstable state? To investigate this, we use a time-dependent data-driven magnetofrictional simulation to model a flux rope eruption of active region AR12473, and systematically perform so-called relaxation runs, i.e., simulations where the driving is stopped at different points in time. The simulations are then continued without driving using both the magnetofrictional model (MFM), and a magnetohydrodynamic (MHD) model for comparison. The flux ropes are extracted with GUITAR (Graphical User Interface for Tracking and Analysing flux Ropes) and analysed in terms of their stability and evolution of characteristic quantities. We find that even between relaxation simulations with eruptive MFRs, the MFR properties can vary greatly depending on the chosen relaxation time for both MFM and MHD. Furthermore, the earliest relaxation time that yields an eruptive MFR is different between MFM and MHD, as is the conclusion on the triggering instability.
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