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Based on the drift-kinetic theory, we develop a model for particleacceleration and transport in solar flares. The model describes the evolutionof the particle distribution function by means of a numerical simulation of thedrift-kinetic Vlasov equation, which allows us to directly compare simulationresults with observations within an actual parameter range of the solar corona.Using this model, we investigate the time evolution of the electrondistribution in a flaring region. The simulation identifies two dominantmechanisms of electron acceleration. One is the betatron acceleration at thetop of closed loops, which enhances the electron velocity perpendicular to themagnetic field line. The other is the inertia drift acceleration in openmagnetic field lines, which produces antisunward electrons. The resultingvelocity space distribution significantly deviates from an isotropicdistribution. The former acceleration can be a generation mechanism ofelectrons that radiate loop-top nonthermal emissions, and the latter be ofescaping electrons from the Sun that should be observed by in-situ measurementsin interplanetary space and resulting radio bursts through plasmainstabilities.

Drift-Kinetic Modeling of Particle Acceleration and Transport in Solar Flares