Speaker
Description
This study investigates the impact of different magnetic field extrapolations on particle acceleration and energy release during solar flares. Using magnetograms obtained before a solar flare event, two distinct magnetic field extrapolations were constructed: a force-free model and a non-force-free model. These models represent different assumptions about the balance of magnetic forces in the solar corona. Magnetohydrodynamic (MHD) simulations were then conducted based on these extrapolations to capture the large-scale dynamics and evolution of the magnetic field during flare events. Subsequently, particle simulations were performed, which were driven by the MHD evolution, enabling analysis of the subsequent particle acceleration processes.
By comparing the outcomes of the simulations based on the two different magnetic field models, the study aims to assess how variations in the magnetic field configuration influence the acceleration of particles and the release of energy during solar flares. This comparison also serves as a foundation for validating the applicability of these models by comparing the results with observed flare behaviour. The findings provide valuable insights into the suitability of force-free versus non-force-free extrapolations in accurately describing flare-related phenomena, and they contribute to refining our understanding of solar flare physics and energy release mechanisms.
