Reduced kinetic approach for modelling energetic particles in the solar corona
Mykola Gordovskyy
University of Manchester
P.K. Browning
Fast magnetic reconnection in solar flares is essentially a kinetic process: non-ideal effects and the energy release are known to be controlled by wave-particle interactions in substantially non-thermal plasma. Still, most studies use the MHD approach for modelling the magnetic reconnection, thus assuming that the plasma is thermal. The main reason for this is that kinetic modelling is extremely computationally expensive.

Recently, we have developed a reduced drift-kinetic approach, based on the assumption that the particle gyro-velocity distribution in nearly thermal (Gordovskyy & Browning, 2016, Arxiv 160200341). This assumption can be justified by our previous large-scale simulations of energy release and particle acceleration in solar flares (e.g. Gordovskyy et al. 2014, A&A 561, 72). This simplification makes it possible to remove the gyro-velocity dimension from the phase space, substituting it by one parameter, perpendicular temperature. Hence, this approach would make it possible to study 2D and, maybe, even 3D large-scale kinetic models with realistic particle parameters, and length- and timescales.