Speaker
Description
We create combined data-based models of magnetic reconnection, and particle acceleration and transport in actual solar flares. This is done by combining 3D MHD simulations initialised using non-linear force-free reconstruction of the coronal magnetic field, with relativistic guiding-centre test-particle simulations of particle acceleration and transport. Using the obtained trajectories for a large number of electrons and protons, we evaluate the locations where the energetic particles precipitate and escape, and calculate bremsstrahlung hard X-ray emission.
Comparison of the results with observations shows that our approach is able to predict some key characteristics of energetic particles in the considered flares, including the locations and relative intensities of hard X-ray and radio emission, as well as locations of helioseismic sources. It can also be used for interpreting in-situ observations of energetic particles in the inner heliosphere by Solar Orbiter and Parker Solar Probe. Hence, the adopted approach can be used for comprehensive observationally-driven modelling of magnetic fields, thermal plasma and non-thermal particles in individual solar flares and their observables.
