Modeling pulses of solar cosmic rays

Abstract

We simulate the transport of particles released from the Sun by the wind program (Ruffolo 1995) in the interplanetary of 1 AU. We find the dense pulses of solar cosmic rays rapidly propagate outward in the strong focusing region near the Sun. Later on, they slowly decay in the diffusion region with increasing distance from the Sun, which is similar to approximate theoretical results of Earl (1976b). We show that one can neglect the effects of motion perpendicular to the magnetic field. We studied the injection profile of cosmic ray particles from the Sun, and found that the duration of particle emission for an impulsive flare has a short duration, but for a gradual flare it has a long duration.