To capture the transient events in accretion flow around black holes, one needs to include the effects from non-thermal electrons. In this presentation I describe the steps I am taking to build a simulation that integrates the trajectories of non-thermal electrons in GRMHD backgrounds. I begin by discussing my results from simulating the magnetic mirroring phenomena of charged particles in a magnetic dipole, in flat and Kerr spacetimes. I also present my most recent results from simulating a collection of particles with constant Lorentz factor and distributed uniformly in direction. My next steps will be to incorporate physically motivated Lorentz factor and direction distributions for an ensemble of particles and couple my simulations to GRMHD backgrounds. This will enable me to simulate a collection of particles distributed in energy and direction and capture their motion within the magnetized flow.
