  Energetic particle populations in the solar corona and in the heliosphere
appear to have different characteristics even when produced in the same solar
flare. It is not clear what causes this difference: properties of the
acceleration region, the large-scale magnetic field configuration in the flare,
or particle transport effects, such as scattering. In this study we use a
combination of magnetohydrodynamic and test-particle approaches to investigate
magnetic reconnection, particle acceleration and transport in two solar flares:
an M-class flare on June 19th, 2013, and an X-class flare on September 6th,
2011. We show that in both events , the same regions are responsible for the
acceleration of particles remaining in the coronal and being ejected towards
the heliosphere. However, the magnetic field structure around the acceleration
region acts as a filter, resulting in different characteristics (such as energy
spectra) acquired by these two populations. We argue that this effect is an
intrinsic property of particle acceleration in the current layers created by
the interchange reconnection and, therefore, may be ubiquitous, particularly,
in non-eruptive solar flares with substantial particle emission into the
heliosphere.
