The Sun’s magnetic field is perpetually being entangled as it is shifted around by convective plasma motion. Magnetic reconnection eventually relaxes the stress accumulated in the entangled magnetic field. A reconnection event may produce electric fields, shocks and turbulence that accelerate charged particles to a significant fraction of the speed of light. Beams of accelerated particles are known to be a key contributor to energy transport in solar flares. While numerical models of energy transport by particle beams in simple 1D atmospheres have provided great insight into the role of accelerated particles, a better understanding of their collective effects in a realistic setting requires 3D models. In this talk, I will discuss our effort to extend the 3D magnetohydrodynamics code Bifrost with a model for accelerated electron beams and show some of the results we have obtained from simulations with the extended code.
This Friday colloquium will be hybrid. Attendees can therefore participate either in-person or via Zoom. Please join via Zoom at
Meeting ID: 690 0104 3754
Attendees will be muted during the colloquium, but will have the opportunity to ask questions at the end by clicking on the "raise hand” button (or send a request via chat).