Monday

While various topological features (e.g. 3D magnetic nulls and separators) have been inferred as likely sites of magnetic reconnection in the solar atmosphere, reconnection is not constrained to solely take place at such sites. In a recent investigation, we studied the particle acceleration resulting from a magnetic reconnection model which causes an arcade of coronal magnetic field to twist and form an erupting flux rope. Crucially, this event takes place in the absence of common topological features where magnetic reconnection is often thought to occur. The results of gyro-averaged particle orbits of electrons and protons for this event can be compared and contrasted with other (often topologically-based) MHD models of magnetic reconnection, revealing several distinct characteristics. We will discuss these, together with aspects of our findings which (unexpectedly) reproduce some general observational features typically seen during two-ribbon flare events.