Particle Acceleration and Transport in Solar Flares
Solar flares are among the most remarkable phenomenon of energy release and particle acceleration in our solar system. A large amount of magnetic energy in the solar corona can be released and converted into non-thermal particles within a few minutes. These high-energy particles produce impulsive non-thermal emissions that are commonly observed, and they can be released into interplanetary space and produce impulsive solar energetic particle events. The non-thermal emissions provide critical diagnostics of the non-thermal particles. Modeling particle acceleration during solar flares is particularly challenging due to the enormous scale separation (kinetic scales < m and global scales >1E8 m) in solar flares.
We have been building a framework for studying particle acceleration during solar flares. Besides the kinetic studies, we are actively working on
- building a numerical model solving the energetic particle transport equations
- studying electron acceleration in the whole flare region (e.g., reconnection and termination shocks)
- producing hard X-ray and microwave emissions from the MHD simulations and the energetic electron maps generated from the model and comparing them with the flare observations
- studying the large-scale transport of energetic electrons in the whole solar eruption regions (SEPs project)