Particle acceleration and their escape into the heliosphere in solar flares with open magnetic field

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.