Speaker
Description
High energy ions and electrons play a crucial role in the fast energy transport in solar flares. A fraction of the particles accelerated in flares precipitate in the solar atmosphere, heating the corona and chromosphere, and producing non-thermal gamma-, X-ray and radio emissions. Others escape from the corona into the heliosphere. The escaping energetic particles are an important component of the space weather.
Recent advances in computational and observational studies of solar energetic particles, have significantly improved our understanding of how particles are transported in the solar corona, and from the corona into the heliosphere, particularly thanks to the unprecedented data from Solar Orbiter and Parker Solar Probe missions. In this talk, I will review the current progress in studies of solar particle acceleration and escape into the heliosphere, with an emphasis on data-constrained computational modelling. I will also present our latest results of magnetic reconnection and particle acceleration modelling in individual solar flares, focusing, in particular, on the effect of magnetic configuration and the location of the acceleration site on the properties of escaping energetic particles.