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Recent observations have shown that coronal shocks driven by coronal massejections can develop and accelerate particles within several solar radii inlarge solar energetic particle (SEP) events. Motivated by this, we present anSEP acceleration study including the process that a fast shock propagatesthrough a streamer-like magnetic field with both closed and open field lines inthe low corona region. The acceleration of protons is modeled by numericallysolving the Parker transport equation with spatial diffusion both along andacross the magnetic field. We show that particles can be sufficientlyaccelerated to up to several hundred MeV within 2-3 solar radii. When the shockpropagates through a streamer-like magnetic field, particles are moreefficiently accelerated compared to the case with a simple radial magneticfield, mainly due to perpendicular shock geometry and the natural trappingeffect of closed magnetic fields. Our results suggest that the coronal magneticfield configuration is an important factor for producing large SEP events. Wefurther show that the coronal magnetic field configuration strongly influencesthe distribution of energetic particles, leading to different locations ofsource regions along the shock front where most of high energy particles areconcentrated. This work may have strong implications to SEP observations. Theupcoming Parker Solar Probe will provide in situ observations for thedistribution of energetic particles in the coronal shock region, and test theresults of the study.

The acceleration of high-energy protons at coronal shocks: the effect of large-scale streamer-like magnetic field structures