Solar flares are efficient particle accelerators and prime laboratories for studying astrophysical acceleration and transport processes. Our understanding of electron acceleration and transport in flares has been enhanced by observationally-driven kinetic modelling and multi-wavelength observations from X-rays to (E)UV to radio. However, many questions remain about how and where energetic...
I will discuss the transport of charged particles in energy- and position-space inside a convection zone-driven 3D turbulent solar corona. It is important to address the formation of the small- and large-scale 3D Current Sheets, the 3D turbulence, and the 3D large scale magnetic disturbances (let us call this environment “3D turbulent reconnection”) in the solar corona before addressing the...
We have carried out the first comprehensive investigation of enhanced line emission from molecular hydrogen, H$_{2}$ at 1333.79 Å, observed at flare ribbons in SOL2014-04-18T13:03. The cool H$_{2}$ emission is known to be fluorescently excited by Si IV 1402.77 Å UV radiation and provides a unique view of the temperature minimum region (TMR). Strong H$_{2}$ emission was observed when the Si IV...
During solar flares, magnetic reconnection unleashes magnetic energy and drives strong electron acceleration and emission within minutes or shorter. Recent multi-wavelength observations (e.g., by EOVSA, RHESSI, and STIX) show that non-thermal radio and hard X-ray emissions could fill up a significant portion of the solar flare region. The electrons responsible for these emissions are thought...
The Sun frequently accelerates near-relativistic electron beams that travel out through the solar corona and interplanetary space, producing type III radio bursts. The formation and motion of type III fine frequency structures is a puzzle but is commonly believed to be related to plasma turbulence in the solar corona and solar wind. Combining a theoretical framework with kinetic simulations...
